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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=Barb%C3%A1%2C+R+H&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Barb%C3%A1%2C+R+H&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Barb%C3%A1%2C+R+H&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Barb%C3%A1%2C+R+H&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </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/2409.03205">arXiv:2409.03205</a> <span> [<a href="https://arxiv.org/pdf/2409.03205">pdf</a>, <a href="https://arxiv.org/format/2409.03205">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/10.1051/0004-6361/202451192">10.1051/0004-6361/202451192 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The YMDB catalog: Young massive detached binaries for the determination of high-precision absolute stellar parameters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mart%C3%ADn-Ravelo%2C+P">Pablo Mart铆n-Ravelo</a>, <a href="/search/astro-ph?searchtype=author&query=Gamen%2C+R">Roberto Gamen</a>, <a href="/search/astro-ph?searchtype=author&query=Arias%2C+J+I">Julia I. Arias</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%C3%A9%2C+A">Andr茅-Nicolas Chen茅</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">Rodolfo H. Barb谩</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="2409.03205v1-abstract-short" style="display: inline;"> Massive stars play a crucial role in the cosmic dynamics and chemical evolution of galaxies, however our understanding of their evolution and properties remains limited. An accurate determination of stellar parameters is essential for advancing our knowledge. Detached eclipsing binaries (DEBs) are particularly valuable for these determinations due to the minimal interaction between their stellar c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.03205v1-abstract-full').style.display = 'inline'; document.getElementById('2409.03205v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.03205v1-abstract-full" style="display: none;"> Massive stars play a crucial role in the cosmic dynamics and chemical evolution of galaxies, however our understanding of their evolution and properties remains limited. An accurate determination of stellar parameters is essential for advancing our knowledge. Detached eclipsing binaries (DEBs) are particularly valuable for these determinations due to the minimal interaction between their stellar components, allowing for precise measurements. This study introduces the Young Massive Detached Binary (YMDB) catalog, designed to address the gap in the high-precision absolute parameter determination for young massive stars. By focusing on DEBs within the spectral range O9-B1, this catalog seeks to provide a reliable database for future studies and improve our understanding of massive star evolution. We conducted a photometric analysis of 87 young massive stars in DEBs using TESS light curves (LCs) that were processed through a custom pipeline. This analysis involved determining the amplitude of magnitude variations, orbital periods, times of minima, eccentricities, and the presence of apsidal motion and heartbeat phenomena. A thorough literature review was performed to obtain MK spectral classifications. We performed our own spectral classification of 19 systems to support the sample where a new classification was lacking or inconclusive. The analysis identified 20 previously unreported binary systems, with 13 newly recognized as variables. Among the 87 stars examined, 30 are confirmed as YMDB members, and 25 are candidates pending spectral classification. The remaining 32 stars belong to unsuitable spectral types or nondetached binary nature. Notable findings include the identification of new LC classifications, eccentricities in 13 systems, and heartbeat phenomena in several targets. The YMDB catalog offers a resource of high-quality LCs and reliable stellar classifications. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.03205v1-abstract-full').style.display = 'none'; document.getElementById('2409.03205v1-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 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">18 pages, 13 figures, 4 tables. Accepted for publication in A&A. Light curves time series and the extended version of Table 2,3,4 will be available on CDS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.21399">arXiv:2407.21399</a> <span> [<a href="https://arxiv.org/pdf/2407.21399">pdf</a>, <a href="https://arxiv.org/format/2407.21399">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> <p class="title is-5 mathjax"> The Villafranca project: Combining Gaia and ground-based surveys to study Galactic OB groups </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Lera%2C+J+A+M">J. A. Molina Lera</a>, <a href="/search/astro-ph?searchtype=author&query=Mart%C3%ADnez%2C+A+L">A. Lambarri Mart铆nez</a>, <a href="/search/astro-ph?searchtype=author&query=Aranda%2C+R+F">R. Fern谩ndez Aranda</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.21399v2-abstract-short" style="display: inline;"> The Villafranca project is studying Galactic stellar groups with OB stars combining information from $Gaia$ and ground-based surveys. We summarize the status of the project and we present its most important results. The Villafranca project has been used to produce a new astrometric calibration for $Gaia$ (E)DR3, which improves the previous one significantly for bright stars. We have discovered tha… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.21399v2-abstract-full').style.display = 'inline'; document.getElementById('2407.21399v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.21399v2-abstract-full" style="display: none;"> The Villafranca project is studying Galactic stellar groups with OB stars combining information from $Gaia$ and ground-based surveys. We summarize the status of the project and we present its most important results. The Villafranca project has been used to produce a new astrometric calibration for $Gaia$ (E)DR3, which improves the previous one significantly for bright stars. We have discovered that dynamical interactions among massive stars at a very young age ($\sim$1 Ma or less) can play a significant interaction in the dynamical evolution of clusters. As a consequence, our current view of the massive-star IMF may be distorted and the number of free-floating neutron stars and black holes higher than previously considered. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.21399v2-abstract-full').style.display = 'none'; document.getElementById('2407.21399v2-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 31 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">To appear in Highlights of Spanish Astrophysics XIII, P254, version with updated style file</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.10167">arXiv:2404.10167</a> <span> [<a href="https://arxiv.org/pdf/2404.10167">pdf</a>, <a href="https://arxiv.org/format/2404.10167">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/10.1126/science.adg7700">10.1126/science.adg7700 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A magnetic massive star has experienced a stellar merger </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Frost%2C+A+J">A. J. Frost</a>, <a href="/search/astro-ph?searchtype=author&query=Sana%2C+H">H. Sana</a>, <a href="/search/astro-ph?searchtype=author&query=Mahy%2C+L">L. Mahy</a>, <a href="/search/astro-ph?searchtype=author&query=Wade%2C+G">G. Wade</a>, <a href="/search/astro-ph?searchtype=author&query=Barron%2C+J">J. Barron</a>, <a href="/search/astro-ph?searchtype=author&query=Bouquin%2C+J+-+L">J. -B. Le Bouquin</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=Schneider%2C+F+R+N">F. R. N. Schneider</a>, <a href="/search/astro-ph?searchtype=author&query=Shenar%2C+T">T. Shenar</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Bowman%2C+D+M">D. M. Bowman</a>, <a href="/search/astro-ph?searchtype=author&query=Fabry%2C+M">M. Fabry</a>, <a href="/search/astro-ph?searchtype=author&query=Farhang%2C+A">A. Farhang</a>, <a href="/search/astro-ph?searchtype=author&query=Marchant%2C+P">P. Marchant</a>, <a href="/search/astro-ph?searchtype=author&query=Morrell%2C+N+I">N. I. Morrell</a>, <a href="/search/astro-ph?searchtype=author&query=Smoker%2C+J+V">J. V. Smoker</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="2404.10167v1-abstract-short" style="display: inline;"> Massive stars (those larger than 8 solar masses at formation) have radiative envelopes that cannot sustain a dynamo, the mechanism that produces magnetic fields in lower-mass stars. Despite this, approximately 7\% of massive stars have observed magnetic fields, the origin of which is debated. We used multi-epoch interferometric and spectroscopic observations to characterize HD 148937, a binary sys… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.10167v1-abstract-full').style.display = 'inline'; document.getElementById('2404.10167v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.10167v1-abstract-full" style="display: none;"> Massive stars (those larger than 8 solar masses at formation) have radiative envelopes that cannot sustain a dynamo, the mechanism that produces magnetic fields in lower-mass stars. Despite this, approximately 7\% of massive stars have observed magnetic fields, the origin of which is debated. We used multi-epoch interferometric and spectroscopic observations to characterize HD 148937, a binary system of two massive stars. We found that only one star is magnetic and that it appears younger than its companion. The system properties and a surrounding bipolar nebula can be reproduced with a model in which two stars merged (in a previous triple system) to produce the magnetic massive star. Our results provide observational evidence that magnetic fields form in at least some massive stars through stellar mergers. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.10167v1-abstract-full').style.display = 'none'; document.getElementById('2404.10167v1-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 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">Full paper with supplementary materials. 59 pages, 18 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Science, 11 Apr 2024, Vol 384, Issue 6692, pp. 214-217 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.12776">arXiv:2207.12776</a> <span> [<a href="https://arxiv.org/pdf/2207.12776">pdf</a>, <a href="https://arxiv.org/format/2207.12776">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/10.1051/0004-6361/202243851">10.1051/0004-6361/202243851 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The IACOB project. VII. The rotational properties of Galactic massive O-type stars revisited </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Holgado%2C+G">G. Holgado</a>, <a href="/search/astro-ph?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/astro-ph?searchtype=author&query=Herrero%2C+A">A. Herrero</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</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="2207.12776v1-abstract-short" style="display: inline;"> Stellar rotation is of key importance for the formation process, evolution, and final fate of massive stars. In this paper we review results from the study of the spin rate properties of a sample of more than 400 Galactic O-type stars surveyed by the IACOB and OWN projects. By combining vsini, Teff, and logg estimates (resulting from a detailed quantitative spectroscopic analysis) with information… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.12776v1-abstract-full').style.display = 'inline'; document.getElementById('2207.12776v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.12776v1-abstract-full" style="display: none;"> Stellar rotation is of key importance for the formation process, evolution, and final fate of massive stars. In this paper we review results from the study of the spin rate properties of a sample of more than 400 Galactic O-type stars surveyed by the IACOB and OWN projects. By combining vsini, Teff, and logg estimates (resulting from a detailed quantitative spectroscopic analysis) with information about the spectroscopic binarity status for an important fraction of the stars in the sample, we provide a renewed overview about how the empirical distribution of projected rotational velocities in the O-star domain depends on mass, evolutionary and binary status. The obtained distributions are then compared with predictions of several state-of-the-art evolutionary models for single stars, as well as from population synthesis simulations including binary interaction, and used to provide hints about the initial velocity distribution of stars with masses in the range ~15-80 Msol. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.12776v1-abstract-full').style.display = 'none'; document.getElementById('2207.12776v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 19 figures, accepted for publication in Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 665, A150 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.04908">arXiv:2206.04908</a> <span> [<a href="https://arxiv.org/pdf/2206.04908">pdf</a>, <a href="https://arxiv.org/ps/2206.04908">ps</a>, <a href="https://arxiv.org/format/2206.04908">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> The Gaia view on massive stars: EDR3 and what to expect from DR3 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez%2C+M+P">M. Pantaleoni Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Weiler%2C+M">M. Weiler</a>, <a href="/search/astro-ph?searchtype=author&query=Reed%2C+B+C">B. C. Reed</a>, <a href="/search/astro-ph?searchtype=author&query=Aranda%2C+R+F">R. Fern谩ndez Aranda</a>, <a href="/search/astro-ph?searchtype=author&query=Bellido%2C+P+C">P. Crespo Bellido</a>, <a href="/search/astro-ph?searchtype=author&query=Sota%2C+A">A. Sota</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">E. J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Lera%2C+J+A+M">J. A. Molina Lera</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="2206.04908v1-abstract-short" style="display: inline;"> At the time of this meeting, the latest Gaia data release is EDR3, published on 3 December 2020, but the next one, DR3, will appear soon, on 13 June 2022. This contribution describes, on the one hand, Gaia EDR3 results on massive stars and young stellar clusters, placing special emphasis on how a correct treatment of the astrometric and photometric calibration yields results that are simultaneousl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.04908v1-abstract-full').style.display = 'inline'; document.getElementById('2206.04908v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.04908v1-abstract-full" style="display: none;"> At the time of this meeting, the latest Gaia data release is EDR3, published on 3 December 2020, but the next one, DR3, will appear soon, on 13 June 2022. This contribution describes, on the one hand, Gaia EDR3 results on massive stars and young stellar clusters, placing special emphasis on how a correct treatment of the astrometric and photometric calibration yields results that are simultaneously precise and accurate. On the other hand, it gives a brief description of the exciting results we can expect from Gaia DR3. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.04908v1-abstract-full').style.display = 'none'; document.getElementById('2206.04908v1-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 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">To appear in Massive Stars Near and Far, Proceedings IAU Symposium No. 361, 2022. N. St-Louis, J. S. Vink & J. Mackey, eds</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.13075">arXiv:2204.13075</a> <span> [<a href="https://arxiv.org/pdf/2204.13075">pdf</a>, <a href="https://arxiv.org/format/2204.13075">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/10.1093/mnras/stac1238">10.1093/mnras/stac1238 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The outer orbit of the high-mass stellar triple system Herschel 36 determined with the VLTI </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sanchez-Bermudez%2C+J">J. Sanchez-Bermudez</a>, <a href="/search/astro-ph?searchtype=author&query=Hummel%2C+C+A">C. A. Hummel</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%ADaz-L%C3%B3pez%2C+J">J. D铆az-L贸pez</a>, <a href="/search/astro-ph?searchtype=author&query=Alberdi%2C+A">A. Alberdi</a>, <a href="/search/astro-ph?searchtype=author&query=Sch%C3%B6del%2C+R">R. Sch枚del</a>, <a href="/search/astro-ph?searchtype=author&query=Arias%2C+J+I">J. I. Arias</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Bastida-Escamilla%2C+E">E. Bastida-Escamilla</a>, <a href="/search/astro-ph?searchtype=author&query=Brandner%2C+W">W. Brandner</a>, <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/astro-ph?searchtype=author&query=Pott%2C+J+-">J. -U. Pott</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2204.13075v1-abstract-short" style="display: inline;"> Multiplicity is a ubiquitous characteristic of massive stars. Multiple systems offer us a unique observational constraint on the formation of high-mass systems. Herschel 36 A is a massive triple system composed of a close binary (Ab1-Ab2) and an outer component (Aa). We measured the orbital motion of the outer component of Herschel 36 A using infrared interferometry with the AMBER and PIONIER inst… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.13075v1-abstract-full').style.display = 'inline'; document.getElementById('2204.13075v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.13075v1-abstract-full" style="display: none;"> Multiplicity is a ubiquitous characteristic of massive stars. Multiple systems offer us a unique observational constraint on the formation of high-mass systems. Herschel 36 A is a massive triple system composed of a close binary (Ab1-Ab2) and an outer component (Aa). We measured the orbital motion of the outer component of Herschel 36 A using infrared interferometry with the AMBER and PIONIER instruments of ESO's Very Large Telescope Interferometer. Our immediate aims are to constrain the masses of all components of this system and to determine if the outer orbit is co-planar with the inner one. Reported spectroscopic data for all three components of this system and our interferometric data allow us to derive full orbital solutions for the outer orbit Aa-Ab and the inner orbit Ab1-Ab2. For the first time, we derive the absolute masses of mAa = 22.3 +/- 1.7 M_sun, mAb1 = 20.5 +/- 1.5 M_sun and mAb2 = 12.5 +/- 0.9 M_sun. Despite not being able to resolve the close binary components, we infer the inclination of their orbit by imposing the same parallax as the outer orbit. Inclinations derived from the inner and outer orbits imply a modest difference of about 22 deg. between the orbital planes. We discuss this result and the formation of Herschel 36 A in the context of Core Accretion and Competitive Accretion models, which make different predictions regarding the statistic of the relative orbital inclinations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.13075v1-abstract-full').style.display = 'none'; document.getElementById('2204.13075v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted to be published by MNRAS, 8 pages, 5 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/2112.02026">arXiv:2112.02026</a> <span> [<a href="https://arxiv.org/pdf/2112.02026">pdf</a>, <a href="https://arxiv.org/format/2112.02026">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4365/ac4414">10.3847/1538-4365/ac4414 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Seventeenth Data Release of the Sloan Digital Sky Surveys: Complete Release of MaNGA, MaStar and APOGEE-2 Data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abdurro%27uf"> Abdurro'uf</a>, <a href="/search/astro-ph?searchtype=author&query=Accetta%2C+K">Katherine Accetta</a>, <a href="/search/astro-ph?searchtype=author&query=Aerts%2C+C">Conny Aerts</a>, <a href="/search/astro-ph?searchtype=author&query=Aguirre%2C+V+S">Victor Silva Aguirre</a>, <a href="/search/astro-ph?searchtype=author&query=Ahumada%2C+R">Romina Ahumada</a>, <a href="/search/astro-ph?searchtype=author&query=Ajgaonkar%2C+N">Nikhil Ajgaonkar</a>, <a href="/search/astro-ph?searchtype=author&query=Ak%2C+N+F">N. Filiz Ak</a>, <a href="/search/astro-ph?searchtype=author&query=Alam%2C+S">Shadab Alam</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+C+A">Carlos Allende Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Almeida%2C+A">Andres Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Anders%2C+F">Friedrich Anders</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+S+F">Scott F. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Andrews%2C+B+H">Brett H. Andrews</a>, <a href="/search/astro-ph?searchtype=author&query=Anguiano%2C+B">Borja Anguiano</a>, <a href="/search/astro-ph?searchtype=author&query=Aquino-Ortiz%2C+E">Erik Aquino-Ortiz</a>, <a href="/search/astro-ph?searchtype=author&query=Aragon-Salamanca%2C+A">Alfonso Aragon-Salamanca</a>, <a href="/search/astro-ph?searchtype=author&query=Argudo-Fernandez%2C+M">Maria Argudo-Fernandez</a>, <a href="/search/astro-ph?searchtype=author&query=Ata%2C+M">Metin Ata</a>, <a href="/search/astro-ph?searchtype=author&query=Aubert%2C+M">Marie Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Avila-Reese%2C+V">Vladimir Avila-Reese</a>, <a href="/search/astro-ph?searchtype=author&query=Badenes%2C+C">Carles Badenes</a>, <a href="/search/astro-ph?searchtype=author&query=Barba%2C+R+H">Rodolfo H. Barba</a>, <a href="/search/astro-ph?searchtype=author&query=Barger%2C+K">Kat Barger</a>, <a href="/search/astro-ph?searchtype=author&query=Barrera-Ballesteros%2C+J+K">Jorge K. Barrera-Ballesteros</a>, <a href="/search/astro-ph?searchtype=author&query=Beaton%2C+R+L">Rachael L. Beaton</a> , et al. (316 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2112.02026v2-abstract-short" style="display: inline;"> This paper documents the seventeenth data release (DR17) from the Sloan Digital Sky Surveys; the fifth and final release from the fourth phase (SDSS-IV). DR17 contains the complete release of the Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey, which reached its goal of surveying over 10,000 nearby galaxies. The complete release of the MaNGA Stellar Library (MaStar) accompanies… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.02026v2-abstract-full').style.display = 'inline'; document.getElementById('2112.02026v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.02026v2-abstract-full" style="display: none;"> This paper documents the seventeenth data release (DR17) from the Sloan Digital Sky Surveys; the fifth and final release from the fourth phase (SDSS-IV). DR17 contains the complete release of the Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey, which reached its goal of surveying over 10,000 nearby galaxies. The complete release of the MaNGA Stellar Library (MaStar) accompanies this data, providing observations of almost 30,000 stars through the MaNGA instrument during bright time. DR17 also contains the complete release of the Apache Point Observatory Galactic Evolution Experiment 2 (APOGEE-2) survey which publicly releases infra-red spectra of over 650,000 stars. The main sample from the Extended Baryon Oscillation Spectroscopic Survey (eBOSS), as well as the sub-survey Time Domain Spectroscopic Survey (TDSS) data were fully released in DR16. New single-fiber optical spectroscopy released in DR17 is from the SPectroscipic IDentification of ERosita Survey (SPIDERS) sub-survey and the eBOSS-RM program. Along with the primary data sets, DR17 includes 25 new or updated Value Added Catalogs (VACs). This paper concludes the release of SDSS-IV survey data. SDSS continues into its fifth phase with observations already underway for the Milky Way Mapper (MWM), Local Volume Mapper (LVM) and Black Hole Mapper (BHM) surveys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.02026v2-abstract-full').style.display = 'none'; document.getElementById('2112.02026v2-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 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">40 pages, 8 figures, 6 tables. In press at ApJSS (arxiv v2 corrects some minor typos and updates references)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2110.08022">arXiv:2110.08022</a> <span> [<a href="https://arxiv.org/pdf/2110.08022">pdf</a>, <a href="https://arxiv.org/format/2110.08022">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"> $胃^1$ Ori C as a medieval bully: a possible very recent ejection in the Trapezium </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez%2C+M+P">M. Pantaleoni Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2110.08022v1-abstract-short" style="display: inline;"> We use Gaia EDR3 astrometry to propose that a dynamical interaction between the multiple system $胃^1$ Ori C and $胃^1$ Ori F ejected the latter as a walkaway star ~1100 years ago (without deceleration) or somewhat later (with a more likely deceleration included). It is unclear whether the final 3-D velocity of $胃^1$ Ori F will be large enough to escape the Orion nebula cluster. </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.08022v1-abstract-full" style="display: none;"> We use Gaia EDR3 astrometry to propose that a dynamical interaction between the multiple system $胃^1$ Ori C and $胃^1$ Ori F ejected the latter as a walkaway star ~1100 years ago (without deceleration) or somewhat later (with a more likely deceleration included). It is unclear whether the final 3-D velocity of $胃^1$ Ori F will be large enough to escape the Orion nebula cluster. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.08022v1-abstract-full').style.display = 'none'; document.getElementById('2110.08022v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted in RNAAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2110.01484">arXiv:2110.01484</a> <span> [<a href="https://arxiv.org/pdf/2110.01484">pdf</a>, <a href="https://arxiv.org/format/2110.01484">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/10.1051/0004-6361/202142366">10.1051/0004-6361/202142366 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Escape from the Bermuda cluster: orphanization by multiple stellar ejections </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez%2C+M+P">M. Pantaleoni Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Weiler%2C+M">M. Weiler</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2110.01484v3-abstract-short" style="display: inline;"> CONTEXT. Dynamical interactions in young stellar clusters can eject massive stars early in their lives and significantly alter their mass functions. If all of the most massive stars are lost, we are left with an orphan cluster. AIMS. We study the Bermuda cluster (Villafranca O-014 NW), the most significant young stellar group in the North America and Pelican nebulae, and the massive stars that m… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.01484v3-abstract-full').style.display = 'inline'; document.getElementById('2110.01484v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.01484v3-abstract-full" style="display: none;"> CONTEXT. Dynamical interactions in young stellar clusters can eject massive stars early in their lives and significantly alter their mass functions. If all of the most massive stars are lost, we are left with an orphan cluster. AIMS. We study the Bermuda cluster (Villafranca O-014 NW), the most significant young stellar group in the North America and Pelican nebulae, and the massive stars that may have been ejected from it to test if it has been orphaned. METHODS. We use Gaia EDR3 parallaxes and proper motions to search for walkaway/runaway stars in the vicinity of the North America and Pelican nebulae. The candidates are analyzed with spectroscopy and photometry to assess their nature and their trajectories are traced back in time to determine at what time they left the Bermuda cluster. RESULTS. We detect three ejection events (Bajamar, Toronto, and HD 201 795 events) that expelled 5, 2, and 2 systems, respectively, or 6, 3, and 3 stars if we count the individual components in spectroscopic/eclipsing binaries. The events took place 1.611$\pm$0.011 Ma, 1.496$\pm$0.044 Ma, and 1.905$\pm$0.037 Ma ago, respectively, but our analysis is marginally consistent with the first two being simultaneous. We detect bow shocks in WISE images associated with four of the ejected systems. Combining the three events, the Bermuda cluster has lost >200 M_Sol, including its three most massive stars, so it can be considered an orphan cluster. One consequence is that the PDMF of the cluster has been radically altered from its top-heavy initial value to one compatible with a Kroupa-like function. Another one is that the cluster is currently expanding with a dynamical time scale consistent with the cause being the ejection events. A scenario in which the Bermuda cluster was formed in a conveyor belt fashion over several hundreds of ka or even 1 Ma is consistent with all the observables. [ABRIDGED] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.01484v3-abstract-full').style.display = 'none'; document.getElementById('2110.01484v3-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 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A. New version after acceptance with some added content suggested by referee</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 657, A72 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2110.01464">arXiv:2110.01464</a> <span> [<a href="https://arxiv.org/pdf/2110.01464">pdf</a>, <a href="https://arxiv.org/format/2110.01464">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/10.1051/0004-6361/202142364">10.1051/0004-6361/202142364 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Villafranca catalog of Galactic OB groups. II. From Gaia DR2 to EDR3 and ten new systems with O stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Aranda%2C+R+F">R. Fern谩ndez Aranda</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez%2C+M+P">M. Pantaleoni Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Bellido%2C+P+C">P. Crespo Bellido</a>, <a href="/search/astro-ph?searchtype=author&query=Sota%2C+A">A. Sota</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">E. J. Alfaro</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2110.01464v2-abstract-short" style="display: inline;"> CONTEXT. This is the second paper of a series on Galactic OB groups that uses astrometric and photometric data from Gaia and spectral classifications from GOSSS and LiLiMaRlin. The previous paper was based on Gaia DR2, this is based on Gaia EDR3. AIMS. The two aims of this paper are to revise the results for the sample from paper I using Gaia EDR3 data and to expand the sample of analyzed stella… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.01464v2-abstract-full').style.display = 'inline'; document.getElementById('2110.01464v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.01464v2-abstract-full" style="display: none;"> CONTEXT. This is the second paper of a series on Galactic OB groups that uses astrometric and photometric data from Gaia and spectral classifications from GOSSS and LiLiMaRlin. The previous paper was based on Gaia DR2, this is based on Gaia EDR3. AIMS. The two aims of this paper are to revise the results for the sample from paper I using Gaia EDR3 data and to expand the sample of analyzed stellar groups to 26, from Villafranca O-001 to Villafranca O-026. METHODS. We use GOSSS to select Galactic stellar groups with O stars and an updated version of the method in paper 0 of this series, combining Gaia EDR3 G+GBP+GRP photometry, positions, proper motions, and parallaxes to assign memberships and measure distances. We present 99 spectra from GOSSS and 32 from LiLiMaRlin for stars in the analyzed groups or in their foreground. RESULTS. We derive distances to the 26 stellar groups with unprecedented precision and accuracy, with total uncertainties <1% within 1 kpc and of ~3% around 3 kpc, values that are almost 4x better than for Gaia DR2. We provide homogeneous spectral types for 110 stars and correct a number of errors in the literature, especially for objects in the Orion nebula cluster. For each of the groups we discuss its membership and present possible runaway/walkaway stars. At least two groups, Villafranca O-O12 S and Villafranca O-014 NW, are orphan clusters in which the most massive stars have been ejected by dynamical interactions, leaving objects with a capped mass function. The existence of such clusters has important consequences for the study of the IMF, the distribution of SNe across the Galaxy, and the population and dynamics of isolated compact objects. We fit PMS isochrones to four clusters to derive ages of 2.0$\pm$0.5 Ma for the sigma Orionis cluster, 4$\pm$2 Ma for NGC 2264, 5.0$\pm$0.5 Ma for NGC 2362, and 8$\pm$2 Ma for the gamma Velorum cluster. [ABRIDGED] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.01464v2-abstract-full').style.display = 'none'; document.getElementById('2110.01464v2-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 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A. Original arXiv version was submitted prior to paper being accepted</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 657, A131 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.13054">arXiv:2109.13054</a> <span> [<a href="https://arxiv.org/pdf/2109.13054">pdf</a>, <a href="https://arxiv.org/format/2109.13054">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/10.1093/mnras/stab2699">10.1093/mnras/stab2699 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Fundamental parameters of the massive eclipsing binary HM1 8 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rodr%C3%ADguez%2C+C+N">Cinthya N. Rodr铆guez</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrero%2C+G+A">Gabriel A. Ferrero</a>, <a href="/search/astro-ph?searchtype=author&query=Benvenuto%2C+O+G">Omar G. Benvenuto</a>, <a href="/search/astro-ph?searchtype=author&query=Gamen%2C+R">Roberto Gamen</a>, <a href="/search/astro-ph?searchtype=author&query=Morrell%2C+N+I">Nidia I. Morrell</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">Rodolfo H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Arias%2C+J">Julia Arias</a>, <a href="/search/astro-ph?searchtype=author&query=Massey%2C+P">Phillip Massey</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="2109.13054v1-abstract-short" style="display: inline;"> We present a comprehensive study of the massive binary system HM1~8, based on multi-epoch high resolution spectroscopy, $V$-band photometry and archival X-ray data. Spectra from the OWN Survey, a high resolution optical monitoring of Southern O and WN stars, are used to analyse the spectral morphology and perform quantitative spectroscopic analysis of both stellar components. The primary and secon… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.13054v1-abstract-full').style.display = 'inline'; document.getElementById('2109.13054v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.13054v1-abstract-full" style="display: none;"> We present a comprehensive study of the massive binary system HM1~8, based on multi-epoch high resolution spectroscopy, $V$-band photometry and archival X-ray data. Spectra from the OWN Survey, a high resolution optical monitoring of Southern O and WN stars, are used to analyse the spectral morphology and perform quantitative spectroscopic analysis of both stellar components. The primary and secondary components are classified as O4.5~IV(f) and O9.7~V, respectively. From a radial-velocity (RV) study we derived a set of orbital parameters for the system. We found an eccentric orbit ($e=0.14 \pm 0.01$) with a period of $P = 5.87820 \pm 0.00008$~days. Through the simultaneous analysis of the RVs and the $V$-band light curve we derived an orbital inclination of $70.0^{\circ} \pm 2.0$ and stellar masses of $M_a=33.6^{+1.4}_{-1.2}~\text{M}_{\sun}$ for the primary, and $M_b=17.7^{+0.5}_{-0.7}~\text{M}_{\sun}$ for the secondary. The components show projected rotational velocities $v_1\sin{i}=105 \pm 14~\text{km~s}^{-1}$ and $v_2\sin{i}=82 \pm 15~\text{km~s}^{-1}$, respectively. A tidal evolution analysis is also performed and found to be in agreement with the orbital characteristics. Finally, the available X-ray observations show no evidence of a colliding winds region, therefore the X-ray emission is attributed to stellar winds. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.13054v1-abstract-full').style.display = 'none'; document.getElementById('2109.13054v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">15 pages, 15 figures, to be published in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.06311">arXiv:2109.06311</a> <span> [<a href="https://arxiv.org/pdf/2109.06311">pdf</a>, <a href="https://arxiv.org/format/2109.06311">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/10.1093/mnras/stac2173">10.1093/mnras/stac2173 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The winking eye of a very massive star: WR 21a revealed as an eclipsing binary by TESS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">Rodolfo H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Gamen%2C+R+C">Roberto C. Gamen</a>, <a href="/search/astro-ph?searchtype=author&query=Mart%C3%ADn-Ravelo%2C+P">Pablo Mart铆n-Ravelo</a>, <a href="/search/astro-ph?searchtype=author&query=Arias%2C+J+I">Julia I. Arias</a>, <a href="/search/astro-ph?searchtype=author&query=Morrell%2C+N+I">Nidia I. Morrell</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="2109.06311v2-abstract-short" style="display: inline;"> WR~21a was known as a massive spectroscopic binary composed of an O2.5 If*/WN6ha primary and an O3 V((f*))z secondary. Although a minimum value, the mass estimated for the primary placed it as one of the most massive stars found in our Galaxy. We report the discovery of photometric variations in the time series observations carried out by the Transiting Exoplanet Survey Satellite (TESS). These lig… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.06311v2-abstract-full').style.display = 'inline'; document.getElementById('2109.06311v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.06311v2-abstract-full" style="display: none;"> WR~21a was known as a massive spectroscopic binary composed of an O2.5 If*/WN6ha primary and an O3 V((f*))z secondary. Although a minimum value, the mass estimated for the primary placed it as one of the most massive stars found in our Galaxy. We report the discovery of photometric variations in the time series observations carried out by the Transiting Exoplanet Survey Satellite (TESS). These light variations are interpreted as formed by two main components: a sharp partial eclipse of the O3 secondary by the O2.5/WN6 star, and tidally excited oscillations. Based on the light minima a new ephemeris for the system is calculated. The system configuration is detached and the observed eclipse corresponds to the periastron passage. During the eclipse, the light curve shape suggests the presence of the heartbeat effect. The frequencies derived for the tidally excited oscillations are harmonics of the orbital period. Combining new and previously published radial velocity measurements, a new spectroscopic orbital solution is also obtained. Using the \textsc{phoebe} code we model the \textit{TESS} light curve and determine stellar radii of $R_{\rm O2.5/WN6}=23.4$ R$_\odot$ and $R_{\rm O3}=14.3$ R$_\odot$ and an orbital inclination $i=62^\circ\!\!.2\pm0^\circ\!\!.9$. The latter combined with the spectroscopic minimum masses lead to absolute masses of $M_{\rm O2.5/WN6}=93.2$ M$_\odot$ and $M_{\rm O3}=52.9$ M$_\odot$, which establishes WR21a as belonging to the rare group of the very massive stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.06311v2-abstract-full').style.display = 'none'; document.getElementById('2109.06311v2-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 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">9 pages, 8 figures, to appear in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.10860">arXiv:2107.10860</a> <span> [<a href="https://arxiv.org/pdf/2107.10860">pdf</a>, <a href="https://arxiv.org/format/2107.10860">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/10.3847/1538-3881/ac1798">10.3847/1538-3881/ac1798 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Double-lined spectroscopic binaries in the APOGEE DR16 and DR17 data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kounkel%2C+M">Marina Kounkel</a>, <a href="/search/astro-ph?searchtype=author&query=Covey%2C+K+R">Kevin R. Covey</a>, <a href="/search/astro-ph?searchtype=author&query=Stassun%2C+K+G">Keivan G. Stassun</a>, <a href="/search/astro-ph?searchtype=author&query=Price-Whelan%2C+A+M">Adrian M. Price-Whelan</a>, <a href="/search/astro-ph?searchtype=author&query=Holtzman%2C+J">Jon Holtzman</a>, <a href="/search/astro-ph?searchtype=author&query=Chojnowski%2C+D">Drew Chojnowski</a>, <a href="/search/astro-ph?searchtype=author&query=Longa-Pe%C3%B1a%2C+P">Pen茅lope Longa-Pe帽a</a>, <a href="/search/astro-ph?searchtype=author&query=Rom%C3%A1n-Z%C3%BA%C3%B1iga%2C+C+G">Carlos G. Rom谩n-Z煤帽iga</a>, <a href="/search/astro-ph?searchtype=author&query=Hernandez%2C+J">Jesus Hernandez</a>, <a href="/search/astro-ph?searchtype=author&query=Serna%2C+J">Javier Serna</a>, <a href="/search/astro-ph?searchtype=author&query=Badenes%2C+C">Carles Badenes</a>, <a href="/search/astro-ph?searchtype=author&query=De+Lee%2C+N">Nathan De Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Majewski%2C+S">Steven Majewski</a>, <a href="/search/astro-ph?searchtype=author&query=Stringfellow%2C+G+S">Guy S. Stringfellow</a>, <a href="/search/astro-ph?searchtype=author&query=Kratter%2C+K+M">Kaitlin M. Kratter</a>, <a href="/search/astro-ph?searchtype=author&query=Moe%2C+M">Maxwell Moe</a>, <a href="/search/astro-ph?searchtype=author&query=Frinchaboy%2C+P+M">Peter M. Frinchaboy</a>, <a href="/search/astro-ph?searchtype=author&query=Beaton%2C+R+L">Rachael L. Beaton</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez-Trincado%2C+J+G">Jos茅 G. Fern谩ndez-Trincado</a>, <a href="/search/astro-ph?searchtype=author&query=Mahadevan%2C+S">Suvrath Mahadevan</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">Dante Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Beers%2C+T+C">Timothy C. Beers</a>, <a href="/search/astro-ph?searchtype=author&query=Schneider%2C+D+P">Donald P. Schneider</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">Rodolfo H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Brownstein%2C+J+R">Joel R. Brownstein</a> , et al. (3 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2107.10860v1-abstract-short" style="display: inline;"> APOGEE spectra offer $\lesssim$1 km s$^{-1}$ precision in the measurement of stellar radial velocities (RVs). This holds even when multiple stars are captured in the same spectrum, as happens most commonly with double-lined spectroscopic binaries (SB2s), although random line of sight alignments of unrelated stars can also occur. We develop a code that autonomously identifies SB2s and higher order… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.10860v1-abstract-full').style.display = 'inline'; document.getElementById('2107.10860v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.10860v1-abstract-full" style="display: none;"> APOGEE spectra offer $\lesssim$1 km s$^{-1}$ precision in the measurement of stellar radial velocities (RVs). This holds even when multiple stars are captured in the same spectrum, as happens most commonly with double-lined spectroscopic binaries (SB2s), although random line of sight alignments of unrelated stars can also occur. We develop a code that autonomously identifies SB2s and higher order multiples in the APOGEE spectra, resulting in 7273 candidate SB2s, 813 SB3s, and 19 SB4s. We estimate the mass ratios of binaries, and for a subset of these systems with sufficient number of measurements we perform a complete orbital fit, confirming that most systems with period $<$10 days have circularized. Overall, we find a SB2 fraction ($F_{SB2}$) $\sim$3\% among main sequence dwarfs, and that there is not a significant trend in $F_{SB2}$ with temperature of a star. We are also able to recover a higher $F_{SB2}$ in sources with lower metallicity, however there are some observational biases. We also examine light curves from TESS to determine which of these spectroscopic binaries are also eclipsing. Such systems, particularly those that are also pre- and post-main sequence, are good candidates for a follow-up analysis to determine their masses and temperatures. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.10860v1-abstract-full').style.display = 'none'; document.getElementById('2107.10860v1-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 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to AJ. 23 pages, 17 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/2106.09451">arXiv:2106.09451</a> <span> [<a href="https://arxiv.org/pdf/2106.09451">pdf</a>, <a href="https://arxiv.org/format/2106.09451">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/10.1093/mnras/stab1769">10.1093/mnras/stab1769 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The GALANTE photometric survey of the northern Galactic plane: Project description and pipeline </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">E. J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Holgado%2C+G">G. Holgado</a>, <a href="/search/astro-ph?searchtype=author&query=Rami%C3%B3%2C+H+V">H. V谩zquez Rami贸</a>, <a href="/search/astro-ph?searchtype=author&query=Varela%2C+J">J. Varela</a>, <a href="/search/astro-ph?searchtype=author&query=Ederoclite%2C+A">A. Ederoclite</a>, <a href="/search/astro-ph?searchtype=author&query=Lorenzo-Guti%C3%A9rrez%2C+A">A. Lorenzo-Guti茅rrez</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=Escudero%2C+H+G">H. Garc铆a Escudero</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa%2C+M">M. Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Coelho%2C+P+R+T">P. R. T. Coelho</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="2106.09451v1-abstract-short" style="display: inline;"> The GALANTE optical photometric survey is observing the northern Galactic plane and some adjacent regions using seven narrow- and intermediate-filters, covering a total of 1618 square degrees. The survey has been designed with multiple exposure times and at least two different air masses per field to maximize its photometric dynamic range, comparable to that of Gaia, and ensure the accuracy of its… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.09451v1-abstract-full').style.display = 'inline'; document.getElementById('2106.09451v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.09451v1-abstract-full" style="display: none;"> The GALANTE optical photometric survey is observing the northern Galactic plane and some adjacent regions using seven narrow- and intermediate-filters, covering a total of 1618 square degrees. The survey has been designed with multiple exposure times and at least two different air masses per field to maximize its photometric dynamic range, comparable to that of Gaia, and ensure the accuracy of its photometric calibration. The goal is to reach at least 1% accuracy and precision in the seven bands for all stars brighter than AB magnitude 17 while detecting fainter stars with lower values of the signal-to-noise ratio.The main purposes of GALANTE are the identification and study of extinguished O+B+WR stars, the derivation of their extinction characteristics, and the cataloguing of F and G stars in the solar neighbourhood. Its data will be also used for a variety of other stellar studies and to generate a high-resolution continuum-free map of the H伪 emission in the Galactic plane. We describe the techniques and the pipeline that are being used to process the data, including the basis of an innovative calibration system based on Gaia DR2 and 2MASS photometry. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.09451v1-abstract-full').style.display = 'none'; document.getElementById('2106.09451v1-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 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.08865">arXiv:2106.08865</a> <span> [<a href="https://arxiv.org/pdf/2106.08865">pdf</a>, <a href="https://arxiv.org/format/2106.08865">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/10.1051/0004-6361/202141018">10.1051/0004-6361/202141018 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MONOS.II. Orbit review and analysis for 35 single-lined spectroscopic binary systems and candidates </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=P%C3%A1ez%2C+E+T">E. Trigueros P谩ez</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Negueruela%2C+I">I. Negueruela</a>, <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/astro-ph?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/astro-ph?searchtype=author&query=Holgado%2C+G">G. Holgado</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="2106.08865v2-abstract-short" style="display: inline;"> [ABRIDGED] AIMS: The MONOS project is collecting information and studying O-type spectroscopic binaries with delta > -20 deg. In this 2nd paper, we tackle the study of the 35 single-line spectroscopic binary (SB1) systems identified in the previous paper of the series (arXiv:1904.11385) by analyzing our data and reviewing the literature orbits of such systems. METHODS: We have measured the radial… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.08865v2-abstract-full').style.display = 'inline'; document.getElementById('2106.08865v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.08865v2-abstract-full" style="display: none;"> [ABRIDGED] AIMS: The MONOS project is collecting information and studying O-type spectroscopic binaries with delta > -20 deg. In this 2nd paper, we tackle the study of the 35 single-line spectroscopic binary (SB1) systems identified in the previous paper of the series (arXiv:1904.11385) by analyzing our data and reviewing the literature orbits of such systems. METHODS: We have measured the radial velocities for the ~700 spectra in our database using two different methods: Gaussian fitting for several diagnostic lines per object and cross-correlation using synthetic spectra. We also explored the TESS database and analyzed the light curves for 31 of the systems. RESULTS: We have confirmed 21 SB1 systems, discarded the binary nature of 6 stars (9 Sge, HD 192 281, HDE 229 232 AB, 68 Cyg, HD 108 and 伪Cam), and left 6 stars as inconclusive due to lack of data. The remaining two stars are 15 Mon Aa which has been classified as SB2, and Cyg OB2-22 C, for which we find evidence that it is most likely a triple system where the O star is orbiting an eclipsing SB1. We have also recalculated 20 new orbital solutions, including the first spectroscopic orbital solution for V747 Cep. For Cyg OB2-22 C we have obtained new ephemerides but no new orbit. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.08865v2-abstract-full').style.display = 'none'; document.getElementById('2106.08865v2-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, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Table 10 and Appendix C are available at the CDS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 655, A4 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2104.03323">arXiv:2104.03323</a> <span> [<a href="https://arxiv.org/pdf/2104.03323">pdf</a>, <a href="https://arxiv.org/format/2104.03323">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/10.1051/0004-6361/202140693">10.1051/0004-6361/202140693 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Tarantula Massive Binary Monitoring V. R 144: a wind-eclipsing binary with a total mass > 140 Msun </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Shenar%2C+T">T. Shenar</a>, <a href="/search/astro-ph?searchtype=author&query=Sana%2C+H">H. Sana</a>, <a href="/search/astro-ph?searchtype=author&query=Marchant%2C+P">P. Marchant</a>, <a href="/search/astro-ph?searchtype=author&query=Pablo%2C+B">B. Pablo</a>, <a href="/search/astro-ph?searchtype=author&query=Richardson%2C+N">N. Richardson</a>, <a href="/search/astro-ph?searchtype=author&query=Moffat%2C+A+F+J">A. F. J. Moffat</a>, <a href="/search/astro-ph?searchtype=author&query=Van+Reeth%2C+T">T. Van Reeth</a>, <a href="/search/astro-ph?searchtype=author&query=Barba%2C+R+H">R. H. Barba</a>, <a href="/search/astro-ph?searchtype=author&query=Bowman%2C+D+M">D. M. Bowman</a>, <a href="/search/astro-ph?searchtype=author&query=Broos%2C+P">P. Broos</a>, <a href="/search/astro-ph?searchtype=author&query=Crowther%2C+P+A">P. A. Crowther</a>, <a href="/search/astro-ph?searchtype=author&query=Clark%2C+J+S">J. S. Clark</a>, <a href="/search/astro-ph?searchtype=author&query=de+Koter%2C+A">A. de Koter</a>, <a href="/search/astro-ph?searchtype=author&query=de+Mink%2C+S+E">S. E. de Mink</a>, <a href="/search/astro-ph?searchtype=author&query=Dsilva%2C+K">K. Dsilva</a>, <a href="/search/astro-ph?searchtype=author&query=Graefener%2C+G">G. Graefener</a>, <a href="/search/astro-ph?searchtype=author&query=Howarth%2C+I+D">I. D. Howarth</a>, <a href="/search/astro-ph?searchtype=author&query=Langer%2C+N">N. Langer</a>, <a href="/search/astro-ph?searchtype=author&query=Mahy%2C+L">L. Mahy</a>, <a href="/search/astro-ph?searchtype=author&query=Apellaniz%2C+J+M">J. Maiz Apellaniz</a>, <a href="/search/astro-ph?searchtype=author&query=Pollock%2C+A+M+T">A. M. T. Pollock</a>, <a href="/search/astro-ph?searchtype=author&query=Schneider%2C+F+R+N">F. R. N. Schneider</a>, <a href="/search/astro-ph?searchtype=author&query=Townsley%2C+L">L. Townsley</a>, <a href="/search/astro-ph?searchtype=author&query=Vink%2C+J+S">J. S. Vink</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="2104.03323v3-abstract-short" style="display: inline;"> R 144 is the visually brightest WR star in the Large Magellanic Cloud (LMC). R 144 was reported to be a binary, making it potentially the most massive binary thus observed. We perform a comprehensive spectral, photometric, orbital, and polarimetric analysis of R 144. R 144 is an eccentric (e=0.51) 74.2-d binary comprising two relatively evolved (age~2 Myr), H-rich WR stars. The hotter primary (W… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.03323v3-abstract-full').style.display = 'inline'; document.getElementById('2104.03323v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2104.03323v3-abstract-full" style="display: none;"> R 144 is the visually brightest WR star in the Large Magellanic Cloud (LMC). R 144 was reported to be a binary, making it potentially the most massive binary thus observed. We perform a comprehensive spectral, photometric, orbital, and polarimetric analysis of R 144. R 144 is an eccentric (e=0.51) 74.2-d binary comprising two relatively evolved (age~2 Myr), H-rich WR stars. The hotter primary (WN5/6h, T=50 kK) and the cooler secondary (WN6/7h,T=45kK) have nearly equal masses. The combination of low rotation and H-depletion observed in the system is well reproduced by contemporary evolution models that include boosted mass-loss at the upper-mass end. The systemic velocity of R 144 and its relative isolation suggest that it was ejected as a runaway from the neighbouring R 136 cluster. The optical light-curve shows a clear orbital modulation that can be well explained as a combination of two processes: excess emission stemming from wind-wind collisions and double wind eclipses. Our light-curve model implies an orbital inclination of i=60.4+-1.5deg, resulting in accurately constrained dynamical masses of 74+-4 and 69+-4 Msun. Assuming that both binary components are core H-burning, these masses are difficult to reconcile with the derived luminosities (logL1,2 = 6.44, 6.39 [Lsun]), which correspond to evolutionary masses of the order of 110 and 100Msun, respectively. Taken at face value, our results imply that both stars have high classical Eddington factors of Gamma_e = 0.78+-0.1. If the stars are on the main sequence, their derived radii (~25Rsun) suggest that they are only slightly inflated, even at this high Eddington factor. Alternatively, the stars could be core-He burning, strongly inflated from the regular size of classical Wolf-Rayet stars (~1Rsun), a scenario that could help resolve the observed mass discrepancy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.03323v3-abstract-full').style.display = 'none'; document.getElementById('2104.03323v3-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 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to A&A on the April 06 2021. 17 pages + 5 page appendix. Version 28.10.2021: corrected typo in Eq. (2); numerator and denominator were inversed on RHS (only typo; no impact on results)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 650, A147 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2103.02748">arXiv:2103.02748</a> <span> [<a href="https://arxiv.org/pdf/2103.02748">pdf</a>, <a href="https://arxiv.org/format/2103.02748">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stab688">10.1093/mnras/stab688 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Alma catalog of OB stars. II. A cross-match with Gaia DR2 and an updated map of the solar neighbourhood </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez%2C+M+P">M. Pantaleoni Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Reed%2C+B+C">B. Cameron Reed</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2103.02748v1-abstract-short" style="display: inline;"> We cross-match the Alma catalog of OB stars with Gaia DR2 astrometry and photometry as a first step towards producing a clean sample of massive stars in the solar neighbourhood with a high degree of completeness. We analyze the resulting colour-absolute magnitude diagram to divide our sample into categories and compare extinction estimates from two sources, finding problems with both of them. The… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.02748v1-abstract-full').style.display = 'inline'; document.getElementById('2103.02748v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.02748v1-abstract-full" style="display: none;"> We cross-match the Alma catalog of OB stars with Gaia DR2 astrometry and photometry as a first step towards producing a clean sample of massive stars in the solar neighbourhood with a high degree of completeness. We analyze the resulting colour-absolute magnitude diagram to divide our sample into categories and compare extinction estimates from two sources, finding problems with both of them. The distances obtained with three different priors are found to have few differences among them, indicating that Gaia DR2 distances are robust. An analysis of the 3-D distribution of massive stars in the solar neighbourhood is presented. We show that a kinematically distinct structure we dub the Cepheus spur extends from the Orion-Cygnus spiral arm towards the Perseus arm and is located above the Galactic mid-plane, likely being related to the recently discovered Radcliffe wave. We propose that this corrugation pattern in the Galactic disk may be responsible for the recent enhanced star formation at its crests and troughs. We also discuss our plans to extend this work in the immediate future. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.02748v1-abstract-full').style.display = 'none'; document.getElementById('2103.02748v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.10206">arXiv:2101.10206</a> <span> [<a href="https://arxiv.org/pdf/2101.10206">pdf</a>, <a href="https://arxiv.org/format/2101.10206">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202140418">10.1051/0004-6361/202140418 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Validation of the accuracy and precision of Gaia EDR3 parallaxes with globular clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez%2C+M+P">M. Pantaleoni Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2101.10206v3-abstract-short" style="display: inline;"> CONTEXT. Gaia EDR3 has produced parallaxes for 1.468x10^9 sources but there are calibration issues that require corrections to the published values and uncertainties. AIMS. We want to characterize the behavior of the uncertainties of the Gaia EDR3 parallaxes. We also aim to provide a procedure for the calculation of distances to stars and stellar clusters. METHODS. We reanalyze some of the data in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.10206v3-abstract-full').style.display = 'inline'; document.getElementById('2101.10206v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.10206v3-abstract-full" style="display: none;"> CONTEXT. Gaia EDR3 has produced parallaxes for 1.468x10^9 sources but there are calibration issues that require corrections to the published values and uncertainties. AIMS. We want to characterize the behavior of the uncertainties of the Gaia EDR3 parallaxes. We also aim to provide a procedure for the calculation of distances to stars and stellar clusters. METHODS. We reanalyze some of the data in the calibration papers for QSO and LMC parallaxes and combine those results with measurements for six bright GCs. We calculate the angular covariance of EDR3 parallaxes at small separations based on the LMC results and combine it with the results for larger angles using QSOs to obtain an analytical formula for the angular covariance over the whole sky. The results for the six GCs are used to validate the parallax bias correction as a function of magnitude, color, and ecliptic latitude and to determine the constant used to convert internal uncertainties to external ones. RESULTS. The angular covariance at zero separation is 106.2 muas^2, yielding a minimum uncertainty for EDR3 parallaxes of 10.3 muas for individual stars. That value can be only slightly reduced for GCs after considering the behavior of the angular covariance of the parallaxes for small separations. The Lindegren et al. parallax bias correction works quite well, except for the brighter magnitudes, suggesting improvements may be possible there. The value of k is 1.1-1.7 and depends on G. Stars with moderately large values of RUWE can still provide useful parallaxes albeit with larger values of k. We give accurate and precise Gaia EDR3 distances to the six GCs and for the specific case of 47 Tuc we are able to beat the angular covariance limit and derive a high-precision distance of 4.53+-0.06 kpc. Finally, a recipe for the derivation of distances to stars and stellar clusters using Gaia EDR3 parallaxes is given. [ABRIDGED] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.10206v3-abstract-full').style.display = 'none'; document.getElementById('2101.10206v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 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">Version accepted 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 649, A13 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2011.12250">arXiv:2011.12250</a> <span> [<a href="https://arxiv.org/pdf/2011.12250">pdf</a>, <a href="https://arxiv.org/format/2011.12250">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/10.1051/0004-6361/202039479">10.1051/0004-6361/202039479 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Lucky spectroscopy, an equivalent technique to Lucky Imaging: II. Spatially-resolved intermediate-resolution blue-violet spectroscopy of 19 close massive binaries using the William Herschel Telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Fari%C3%B1a%2C+C">C. Fari帽a</a>, <a href="/search/astro-ph?searchtype=author&query=Sota%2C+A">A. Sota</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez%2C+M+P">M. Pantaleoni Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Holgado%2C+G">G. Holgado</a>, <a href="/search/astro-ph?searchtype=author&query=Negueruela%2C+I">I. Negueruela</a>, <a href="/search/astro-ph?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</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="2011.12250v1-abstract-short" style="display: inline;"> CONTEXT. Many massive stars have nearby companions whose presence hamper their characterization through spectroscopy. AIMS. We want to continue obtaining spatially resolved spectroscopy of close massive visual binaries to derive their spectral types. METHODS. We have used lucky spectroscopy to obtain many short long-slit spectroscopic exposures of 19 close visual binaries under good seeing conditi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.12250v1-abstract-full').style.display = 'inline'; document.getElementById('2011.12250v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.12250v1-abstract-full" style="display: none;"> CONTEXT. Many massive stars have nearby companions whose presence hamper their characterization through spectroscopy. AIMS. We want to continue obtaining spatially resolved spectroscopy of close massive visual binaries to derive their spectral types. METHODS. We have used lucky spectroscopy to obtain many short long-slit spectroscopic exposures of 19 close visual binaries under good seeing conditions. We selected those with the best characteristics, extracted the spectra using multiple-profile fitting, and combined the results to derive spatially separated spectra. The results are analyzed in combination with data from lucky imaging, regular intermediate-resolution single-order spectroscopy, and 茅chelle high-resolution spectroscopy. RESULTS. The new application of lucky spectroscopy has allowed us to [a] spatially disentangle for the first time two O stars (FN CMa B and 6 Cas B) with brighter BA supergiant companions; [b] determine that two B stars (alpha Sco B and HD 164492 B) with close and more massive companions are fast rotators; [c] extend the technique to cases with extreme magnitude differences, shorter separations, and fainter primary magnitudes down to B=11; [d] spatially disentangle the spectra of stars with companions as diverse as an A supergiant (6 Cas A), a WR star (WR 157), and an M supergiant (alpha Sco A); [e] discover the unexpected identity of some targets such as two previously unknown bright O stars (HD 51756 B and BD +60 544) and a new member of the rare OC category (HD 8768 A); and [f] identify and classify which of the components of four visual binaries is a double-lined spectroscopic binary and for another seven systems detect signs of spectroscopic binarity using high-spectral-resolution spectroscopy. We also present a determination of the limits of the technique. [ABRIDGED] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.12250v1-abstract-full').style.display = 'none'; document.getElementById('2011.12250v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">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, A11 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2010.02113">arXiv:2010.02113</a> <span> [<a href="https://arxiv.org/pdf/2010.02113">pdf</a>, <a href="https://arxiv.org/format/2010.02113">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/10.1051/0004-6361/202039233">10.1051/0004-6361/202039233 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> VVVX-Gaia Discovery of a Low Luminosity Globular Cluster in the Milky Way Disk </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Garro%2C+E+R">E. R. Garro</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%B3mez%2C+M">M. G贸mez</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso-Garc%C3%ADa%2C+J">J. Alonso-Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">B. Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=Clari%C3%A1%2C+J+J">J. J. Clari谩</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%C3%A9%2C+A+N">A. N. Chen茅</a>, <a href="/search/astro-ph?searchtype=author&query=Dias%2C+B">B. Dias</a>, <a href="/search/astro-ph?searchtype=author&query=Hempel%2C+M">M. Hempel</a>, <a href="/search/astro-ph?searchtype=author&query=Ivanov%2C+V+D">V. D. Ivanov</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+P+W">P. W. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=Majaess%2C+D">D. Majaess</a>, <a href="/search/astro-ph?searchtype=author&query=Mauro%2C+F">F. Mauro</a>, <a href="/search/astro-ph?searchtype=author&query=Bidin%2C+C+M">C. Moni Bidin</a>, <a href="/search/astro-ph?searchtype=author&query=Palma%2C+T">T. Palma</a>, <a href="/search/astro-ph?searchtype=author&query=Pullen%2C+J+B">J. B. Pullen</a>, <a href="/search/astro-ph?searchtype=author&query=Saito%2C+R+K">R. K. Saito</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+L">L. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Surot%2C+F">F. Surot</a>, <a href="/search/astro-ph?searchtype=author&query=Alegr%C3%ADa%2C+S+R">S. Ram铆rez Alegr铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">M. Rejkuba</a>, <a href="/search/astro-ph?searchtype=author&query=Ripepi%2C+V">V. Ripepi</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="2010.02113v1-abstract-short" style="display: inline;"> Milky Way globular clusters (MW GCs) are difficult to identify at low Galactic latitudes because of high differential extinction and heavy star crowding. The new deep near-IR images and photometry from the VISTA Variables in the Via L谩ctea Extended Survey (VVVX) allow us to chart previously unexplored regions. Our long term aim is to complete the census of MW GCs. The immediate goals are to estima… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.02113v1-abstract-full').style.display = 'inline'; document.getElementById('2010.02113v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.02113v1-abstract-full" style="display: none;"> Milky Way globular clusters (MW GCs) are difficult to identify at low Galactic latitudes because of high differential extinction and heavy star crowding. The new deep near-IR images and photometry from the VISTA Variables in the Via L谩ctea Extended Survey (VVVX) allow us to chart previously unexplored regions. Our long term aim is to complete the census of MW GCs. The immediate goals are to estimate the astrophysical parameters, measuring their reddenings, extinctions, distances, total luminosities, proper motions, sizes, metallicities and ages. We use the near-IR VVVX survey database, in combination with Gaia DR2 optical photometry, and with the Two Micron All Sky Survey (2MASS) photometry. We report the detection of a heretofore unknown Galactic Globular Cluster at $RA =$ 14:09:00.0; $DEC=-$65:37:12 (J2000). We calculate a reddening of $E(J-K_s)=(0.3\pm 0.03)$ mag and an extinction of $A_{K_s}=(0.15\pm 0.01)$ mag for this new GC. Its distance modulus and corresponding distance were measured as $(m-M)=(15.93\pm0.03)$ mag and $D=(15.5\pm1.0)$ kpc, respectively. We estimate the metallicity and age by comparison with known GCs and by fitting PARSEC and Dartmouth isochrones, finding $[Fe/H]=(-0.70\pm0.2)$ dex and $t=(11.0\pm1.0)$ Gyr. The mean GC PMs from Gaia are $渭_{伪^\ast}=(-4.68 \pm 0.47 )$ mas $yr^{-1}$ and $渭_未=(-1.34 \pm 0.45)$ mas $yr^{-1}$. The total luminosity of our cluster is estimated to be $M_{Ks}=(-7.76\pm 0.5)$ mag. We have found a new low-luminosity, old and metal-rich globular cluster, situated in the far side of the Galactic disk, at $R_{G}=11.2$ kpc from the Galactic centre, and at $z=1.0$ kpc below the plane. Interestingly, the location, metallicity and age of this globular cluster are coincident with the Monoceros Ring (MRi) structure. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.02113v1-abstract-full').style.display = 'none'; document.getElementById('2010.02113v1-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 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 642, L19 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2009.05773">arXiv:2009.05773</a> <span> [<a href="https://arxiv.org/pdf/2009.05773">pdf</a>, <a href="https://arxiv.org/format/2009.05773">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/10.1051/0004-6361/202038228">10.1051/0004-6361/202038228 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Villafranca catalog of Galactic OB groups: I. Systems with O2-O3.5 stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/astro-ph?searchtype=author&query=Bellido%2C+P+C">P. Crespo Bellido</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Aranda%2C+R+F">R. Fern谩ndez Aranda</a>, <a href="/search/astro-ph?searchtype=author&query=Sota%2C+A">A. Sota</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2009.05773v1-abstract-short" style="display: inline;"> CONTEXT. The GOSSS spectral classifications and Gaia data have significantly improved our ability to measure distances and determine memberships of stellar groups with OB stars. AIMS. We have started a program to identify, measure distances, and determine the membership of Galactic stellar groups with OB stars. We start with the identification and distance determinations of groups with O stars. In… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.05773v1-abstract-full').style.display = 'inline'; document.getElementById('2009.05773v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.05773v1-abstract-full" style="display: none;"> CONTEXT. The GOSSS spectral classifications and Gaia data have significantly improved our ability to measure distances and determine memberships of stellar groups with OB stars. AIMS. We have started a program to identify, measure distances, and determine the membership of Galactic stellar groups with OB stars. We start with the identification and distance determinations of groups with O stars. In this paper we concentrate on groups that contain stars with the earliest spectral subtypes. METHODS. We use GOSSS to select Galactic stellar groups with O2-O3.5 stars and a method that combines Gaia DR2 photometry, positions, proper motions, and parallaxes to assign robust memberships and measure distances. We also include the two clusters in that paper to generate our first list of 16 O-type Galactic stellar groups. RESULTS. We derive distances, determine the membership, and analyze the structure of sixteen Galactic stellar groups with O stars, Villafranca O-001 to O-016, including the 14 groups with the earliest-O-type optically-accessible stars known in the Milky Way. We compare our distance with previous results and establish that the best consistency is with VLBI parallaxes and the worst is with kinematic distances. Our results indicate that massive stars can form in relatively low-mass clusters or even in near-isolation, as is the case for the Bajamar star in the North America nebula. This lends support to the hierarchical scenario of star formation, where some stars are born in well-defined bound clusters but others are born in associations that are unbound from the beginning: groups of newborn stars come in many shapes and sizes. We propose that HD 64 568 and HD 64 315 AB could have been ejected simultaneously from Villafranca O-012 S. Our results are consistent with a difference of approx. 20 microas in the Gaia DR2 parallax zero point between bright and faint stars. (ABRIDGED) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.05773v1-abstract-full').style.display = 'none'; document.getElementById('2009.05773v1-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 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">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 643, A138 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2008.00834">arXiv:2008.00834</a> <span> [<a href="https://arxiv.org/pdf/2008.00834">pdf</a>, <a href="https://arxiv.org/format/2008.00834">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/staa2371">10.1093/mnras/staa2371 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galactic extinction laws: II. Hidden in plain sight, a new interstellar absorption band at 7700 脜 broader than any known DIB </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Caballero%2C+J+A">J. A. Caballero</a>, <a href="/search/astro-ph?searchtype=author&query=Bohlin%2C+R+C">R. C. Bohlin</a>, <a href="/search/astro-ph?searchtype=author&query=Fari%C3%B1a%2C+C">C. Fari帽a</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2008.00834v1-abstract-short" style="display: inline;"> We have detected a broad interstellar absorption band centred close to 7700 脜 and with a FWHM of 176.6$\pm$3.9 脜. This is the first such absorption band detected in the optical range and is significantly wider than the numerous diffuse interstellar bands (DIBs). It remained undiscovered until now because it is partially hidden behind the A telluric band produced by O$_2$. The band was discovered u… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.00834v1-abstract-full').style.display = 'inline'; document.getElementById('2008.00834v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.00834v1-abstract-full" style="display: none;"> We have detected a broad interstellar absorption band centred close to 7700 脜 and with a FWHM of 176.6$\pm$3.9 脜. This is the first such absorption band detected in the optical range and is significantly wider than the numerous diffuse interstellar bands (DIBs). It remained undiscovered until now because it is partially hidden behind the A telluric band produced by O$_2$. The band was discovered using STIS@HST spectra and later detected in a large sample of stars of diverse type (OB stars, BA supergiants, red giants) using further STIS and ground-based spectroscopy. The EW of the band is measured and compared with our extinction and K I $位位$7667.021,7701.093 measurements for the same sample. The carrier is ubiquitous in the diffuse and translucent Galactic ISM but is depleted in the environment around OB stars. In particular, it appears to be absent or nearly so in sightlines rich in molecular carbon. This behaviour is similar to that of the $蟽$-type DIBs, which originate in the low/intermediate-density UV-exposed ISM but are depleted in the high-density UV-shielded molecular clouds. We also present an update on our previous work on the relationship between $E(4405-5495)$ and $R_{5495}$ and incorporate our results into a general model of the ISM. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.00834v1-abstract-full').style.display = 'none'; document.getElementById('2008.00834v1-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 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">17 pages, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2006.09206">arXiv:2006.09206</a> <span> [<a href="https://arxiv.org/pdf/2006.09206">pdf</a>, <a href="https://arxiv.org/format/2006.09206">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/staa1790">10.1093/mnras/staa1790 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galactic extinction laws: I. A global NIR analysis with 2MASS photometry </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez%2C+M+P">M. Pantaleoni Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</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=Nogueras-Lara%2C+F">F. Nogueras-Lara</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="2006.09206v1-abstract-short" style="display: inline;"> We have started an ambitious program to determine if the full diversity of extinction laws is real or if some of it is due to calibration or methodological issues. Here we start by analyzing the information on NIR extinction in a 2MASS stellar sample with good quality photometry and very red colours. We calculate the extinction at 1 $渭$m, $A_1$, and the power-law exponent, $伪$ ($A_位= A_1 位^{-伪}$),… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.09206v1-abstract-full').style.display = 'inline'; document.getElementById('2006.09206v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2006.09206v1-abstract-full" style="display: none;"> We have started an ambitious program to determine if the full diversity of extinction laws is real or if some of it is due to calibration or methodological issues. Here we start by analyzing the information on NIR extinction in a 2MASS stellar sample with good quality photometry and very red colours. We calculate the extinction at 1 $渭$m, $A_1$, and the power-law exponent, $伪$ ($A_位= A_1 位^{-伪}$), for the 2MASS stars located in the extinction trajectory in the $H-K$ vs. $J-H$ plane expected for red giants with $A_1 > 5$ mag. We test the validity of the assumption about the nature of those stars, whether a single or multiple values of $伪$ are needed, and the spatial variations of the results. Most ($\sim$83%) of those stars can indeed be explained by high-extinction red giants and the rest is composed of extinguished AGB stars (mostly O-rich), blended sources, and smaller numbers of other objects, a contaminant fraction that can be reduced with the help of Gaia} DR2 data. Galactic red giants experience a NIR extinction with $伪\sim 2.27$ and an uncertainty of a few hundredths of a magnitude. There is no significant spread in $伪$ even though our sample is widely distributed and has a broad range of extinctions. Differences with previous results are ascribed to the treatment of non-linear photometric effects and/or the contaminant correction. Future research should concentrate in finding the correct functional form for the NIR extinction law. In the appendix we detail the treatment of non-linear photometric effects in the 2MASS bands. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.09206v1-abstract-full').style.display = 'none'; document.getElementById('2006.09206v1-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 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">13 pages, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2005.09658">arXiv:2005.09658</a> <span> [<a href="https://arxiv.org/pdf/2005.09658">pdf</a>, <a href="https://arxiv.org/format/2005.09658">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/10.1051/0004-6361/202037700">10.1051/0004-6361/202037700 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Variability of OB stars from TESS southern Sectors 1-13 and high-resolution IACOB and OWN spectroscopy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Burssens%2C+S">S. Burssens</a>, <a href="/search/astro-ph?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/astro-ph?searchtype=author&query=Bowman%2C+D+M">D. M. Bowman</a>, <a href="/search/astro-ph?searchtype=author&query=Holgado%2C+G">G. Holgado</a>, <a href="/search/astro-ph?searchtype=author&query=Michielsen%2C+M">M. Michielsen</a>, <a href="/search/astro-ph?searchtype=author&query=de+Burgos%2C+A">A. de Burgos</a>, <a href="/search/astro-ph?searchtype=author&query=Castro%2C+N">N. Castro</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Aerts%2C+C">C. Aerts</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="2005.09658v2-abstract-short" style="display: inline;"> Lack of high-precision long-term continuous photometric data for large samples of stars has prevented the large-scale exploration of pulsational variability in the OB star regime. As a result, the candidates for in-depth asteroseismic modelling remained limited to a few tens of dwarfs. The TESS nominal space mission has surveyed the southern sky, yielding continuous data of at least 27 d for hundr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.09658v2-abstract-full').style.display = 'inline'; document.getElementById('2005.09658v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2005.09658v2-abstract-full" style="display: none;"> Lack of high-precision long-term continuous photometric data for large samples of stars has prevented the large-scale exploration of pulsational variability in the OB star regime. As a result, the candidates for in-depth asteroseismic modelling remained limited to a few tens of dwarfs. The TESS nominal space mission has surveyed the southern sky, yielding continuous data of at least 27 d for hundreds of OB stars. We aim to couple TESS data in the southern sky with spectroscopy to study the variability over mass and evolution. We focus mainly on the presence of coherent pulsation modes that may or may not be present in the theoretical instability domains and unravel all frequency behaviour in the amplitude spectra of the TESS data. We compose a sample of 98 OB-type stars observed by TESS in Sectors 1-13 and with available high-resolution spectroscopy gathered by the IACOB and OWN surveys. We present the short-cadence 2-min light curves of dozens of OB-type stars, that have one or more spectra in the IACOB or OWN database. Based on these light curves and their Lomb-Scargle periodograms we perform variability classification and frequency analysis, and place the stars in the spectroscopic Hertzsprung-Russell diagram to interpret the variability in an evolutionary context. We deduce diverse origins of the variability found in all of the 98 OB stars in the TESS data. Among these we find several new variable stars, including three hybrid pulsators, three eclipsing binaries, high frequency modes in a Be star, and potential heat-driven pulsations in two Oe stars. We identify stars for which future asteroseismic modelling is possible, provided mode identification is achieved. By comparing the position of the variables to theoretical instability strips we discuss the current shortcomings in non-adiabatic pulsation theory, and the distribution of pulsators in the upper Hertzsprung-Russell diagram. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.09658v2-abstract-full').style.display = 'none'; document.getElementById('2005.09658v2-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 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 May, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A. 18(+47) pages, 15(+100) figures, 3(+2) tables. Language edited and typos removed. Fig. 3, 14, 15 corrected for small plotting error (results unchanged)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 639, A81 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2005.05446">arXiv:2005.05446</a> <span> [<a href="https://arxiv.org/pdf/2005.05446">pdf</a>, <a href="https://arxiv.org/format/2005.05446">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/10.1051/0004-6361/202037699">10.1051/0004-6361/202037699 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The IACOB project. VI. On the elusive detection of massive O-type stars close to the ZAMS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Holgado%2C+G">G. Holgado</a>, <a href="/search/astro-ph?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/astro-ph?searchtype=author&query=Haemmerl%C3%A9%2C+L">L. Haemmerl茅</a>, <a href="/search/astro-ph?searchtype=author&query=Lennon%2C+D+J">D. J. Lennon</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Cervi%C3%B1o%2C+M">M. Cervi帽o</a>, <a href="/search/astro-ph?searchtype=author&query=Castro%2C+N">N. Castro</a>, <a href="/search/astro-ph?searchtype=author&query=Herrero%2C+A">A. Herrero</a>, <a href="/search/astro-ph?searchtype=author&query=Meynet%2C+G">G. Meynet</a>, <a href="/search/astro-ph?searchtype=author&query=Arias%2C+J+I">J. I. Arias</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="2005.05446v3-abstract-short" style="display: inline;"> The apparent lack of massive O-type stars near the zero-age main sequence (at ages < 2 Myr) is a topic widely discussed. Different explanations for this elusive detection have been proposed, but no firm conclusions have been reached yet. We reassess this empirical result benefiting from the high-quality spectroscopic observations of >400 Galactic O-type stars gathered by the IACOB and OWN surveys.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.05446v3-abstract-full').style.display = 'inline'; document.getElementById('2005.05446v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2005.05446v3-abstract-full" style="display: none;"> The apparent lack of massive O-type stars near the zero-age main sequence (at ages < 2 Myr) is a topic widely discussed. Different explanations for this elusive detection have been proposed, but no firm conclusions have been reached yet. We reassess this empirical result benefiting from the high-quality spectroscopic observations of >400 Galactic O-type stars gathered by the IACOB and OWN surveys. We used temperatures and gravities from a iacob-gbat/fastwind spectroscopic analysis to locate our sample in the Kiel and spectroscopic HR diagrams. We evaluated the completeness of our sample of stars, observational biases using information from the Galactic O star catalog (GOSC), systematics of our methodology, and compare with other recent studies using smaller samples of Galactic O-type stars. We base our discussion on the spectroscopic HR diagram to avoid the use of uncertain distances. We performed a detailed study of the young cluster Trumpler-14 as an example of how Gaia cluster distances can help to construct the associated classical HR diagram. The apparent lack of massive O-type stars near the ZAMS with masses between 30 and 70 Msol persist even when spectroscopic results from a large, non-biased sample of stars are used. We do not find correlation between the dearth of stars and observational biases, limitations of our methodology, or the use of spectroscopic HR diagram instead of the classical one. Investigating the efficiency of mass accretion during the formation process we conclude that an adjustment of the accretion rate towards lower values could reconcile the hotter boundary of detected O-type stars and the theoretical birthline. Last, we discuss that the presence of a small sample of O2-O3.5 stars found closer to the ZAMS might be explained taking into account non-standard star evolution (e.g. binary interaction, mergers, or homogeneous evolution). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.05446v3-abstract-full').style.display = 'none'; document.getElementById('2005.05446v3-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 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 May, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 15 figures, accepted for publication in Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 638, A157 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2004.10032">arXiv:2004.10032</a> <span> [<a href="https://arxiv.org/pdf/2004.10032">pdf</a>, <a href="https://arxiv.org/format/2004.10032">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/staa1156">10.1093/mnras/staa1156 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The high-energy emission from HD~93129A near periastron </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=del+Palacio%2C+S">S. del Palacio</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa%2C+F">F. Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Altamirano%2C+D">D. Altamirano</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Bosch-Ramon%2C+V">V. Bosch-Ramon</a>, <a href="/search/astro-ph?searchtype=author&query=Corcoran%2C+M">M. Corcoran</a>, <a href="/search/astro-ph?searchtype=author&query=De+Becker%2C+M">M. De Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Hamaguchi%2C+K">K. Hamaguchi</a>, <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/astro-ph?searchtype=author&query=Adrover%2C+P+M">P. Munar Adrover</a>, <a href="/search/astro-ph?searchtype=author&query=Paredes%2C+J+M">J. M. Paredes</a>, <a href="/search/astro-ph?searchtype=author&query=Romero%2C+G+E">G. E. Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Sana%2C+H">H. Sana</a>, <a href="/search/astro-ph?searchtype=author&query=Tavani%2C+M">M. Tavani</a>, <a href="/search/astro-ph?searchtype=author&query=ud-Doula%2C+A">A. ud-Doula</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2004.10032v1-abstract-short" style="display: inline;"> We conducted an observational campaign towards one of the most massive and luminous colliding wind binaries in the Galaxy, HD~93129A, close to its periastron passage in 2018. During this time the source was predicted to be in its maximum of high-energy emission. Here we present our data analysis from the X-ray satellites \textit{Chandra} and \textit{NuSTAR} and the $纬$-ray satellite \textit{AGILE}… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.10032v1-abstract-full').style.display = 'inline'; document.getElementById('2004.10032v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2004.10032v1-abstract-full" style="display: none;"> We conducted an observational campaign towards one of the most massive and luminous colliding wind binaries in the Galaxy, HD~93129A, close to its periastron passage in 2018. During this time the source was predicted to be in its maximum of high-energy emission. Here we present our data analysis from the X-ray satellites \textit{Chandra} and \textit{NuSTAR} and the $纬$-ray satellite \textit{AGILE}. High-energy emission coincident with HD~93129A was detected in the X-ray band up to $\sim$18~keV, whereas in the $纬$-ray band only upper limits were obtained. We interpret the derived fluxes using a non-thermal radiative model for the wind-collision region. We establish a conservative upper limit for the fraction of the wind kinetic power that is converted into relativistic electron acceleration, $f_\mathrm{NT,e} < 0.02$. In addition, we set a lower limit for the magnetic field in the wind-collision region as $B_\mathrm{WCR} > 0.3$~G. We also argue a putative interpretation of the emission from which we estimate $f_\mathrm{NT,e} \approx 0.006$ and $B_\mathrm{WCR} \approx 0.5$~G. We conclude that multi-wavelength, dedicated observing campaigns during carefully selected epochs are a powerful tool for characterising the relativistic particle content and magnetic field intensity in colliding wind binaries. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.10032v1-abstract-full').style.display = 'none'; document.getElementById('2004.10032v1-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 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 10 figures, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2002.12149">arXiv:2002.12149</a> <span> [<a href="https://arxiv.org/pdf/2002.12149">pdf</a>, <a href="https://arxiv.org/format/2002.12149">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/10.1051/0004-6361/202037730">10.1051/0004-6361/202037730 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Spatially resolved spectroscopy of close massive visual binaries with HST/STIS: I. Seven O-type systems </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</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="2002.12149v1-abstract-short" style="display: inline;"> CONTEXT. Many O-type stars have nearby companions whose presence hamper their characterization through spectroscopy. AIMS. We want to obtain spatially resolved spectroscopy of close O-type visual binaries to derive their spectral types. METHODS. We use the Space Telescope Imaging Spectrograph (STIS) of the Hubble Space Telescope (HST) to obtain long-slit blue-violet spectroscopy of eight Galac… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.12149v1-abstract-full').style.display = 'inline'; document.getElementById('2002.12149v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2002.12149v1-abstract-full" style="display: none;"> CONTEXT. Many O-type stars have nearby companions whose presence hamper their characterization through spectroscopy. AIMS. We want to obtain spatially resolved spectroscopy of close O-type visual binaries to derive their spectral types. METHODS. We use the Space Telescope Imaging Spectrograph (STIS) of the Hubble Space Telescope (HST) to obtain long-slit blue-violet spectroscopy of eight Galactic O-type stars with nearby visual companions and use spatial-profile fitting to extract the separate spectra. We also use the ground-based Galactic O-Star Spectroscopic Survey (GOSSS) to study more distant visual components. RESULTS. We spatially resolve seven of the eight systems, present spectra for their components, and obtain their spectral types. Those seven multiple systems are iota Ori Aa,Ab,B, 15 Mon Aa,Ab,C, tau CMa Aa,Ab,B,C,D,E, HD 206 267 Aa,Ab,C,D, HD 193 443 A,B, HD 16 429 Aa,Ab, and IU Aur A,B. This is the first time that spatially resolved spectroscopy of the close visual binaries of those systems is obtained. We establish the applicability of the technique as a function of the separation and magnitude difference of the binary. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.12149v1-abstract-full').style.display = 'none'; document.getElementById('2002.12149v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 February, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 636, A28 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2002.02690">arXiv:2002.02690</a> <span> [<a href="https://arxiv.org/pdf/2002.02690">pdf</a>, <a href="https://arxiv.org/format/2002.02690">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/10.1051/0004-6361/201936361">10.1051/0004-6361/201936361 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> VLT/X-shooter spectroscopy of massive young stellar objects in the 30 Doradus region of the Large Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=van+Gelder%2C+M+L">M. L. van Gelder</a>, <a href="/search/astro-ph?searchtype=author&query=Kaper%2C+L">L. Kaper</a>, <a href="/search/astro-ph?searchtype=author&query=Japelj%2C+J">J. Japelj</a>, <a href="/search/astro-ph?searchtype=author&query=Ram%C3%ADrez-Tannus%2C+M+C">M. C. Ram铆rez-Tannus</a>, <a href="/search/astro-ph?searchtype=author&query=Ellerbroek%2C+L+E">L. E. Ellerbroek</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Bestenlehner%2C+J+M">J. M. Bestenlehner</a>, <a href="/search/astro-ph?searchtype=author&query=Bik%2C+A">A. Bik</a>, <a href="/search/astro-ph?searchtype=author&query=Gr%C3%A4fener%2C+G">G. Gr盲fener</a>, <a href="/search/astro-ph?searchtype=author&query=de+Koter%2C+A">A. de Koter</a>, <a href="/search/astro-ph?searchtype=author&query=de+Mink%2C+S+E">S. E. de Mink</a>, <a href="/search/astro-ph?searchtype=author&query=Sabbi%2C+E">E. Sabbi</a>, <a href="/search/astro-ph?searchtype=author&query=Sana%2C+H">H. Sana</a>, <a href="/search/astro-ph?searchtype=author&query=Sewi%C5%82o%2C+M">M. Sewi艂o</a>, <a href="/search/astro-ph?searchtype=author&query=Vink%2C+J+S">J. S. Vink</a>, <a href="/search/astro-ph?searchtype=author&query=Walborn%2C+N+R">N. R. Walborn</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="2002.02690v1-abstract-short" style="display: inline;"> The process of massive star ($M\geq8~M_\odot$) formation is still poorly understood. Observations of massive young stellar objects (MYSOs) are challenging due to their rarity, short formation timescale, large distances, and high circumstellar extinction. Here, we present the results of a spectroscopic analysis of a population of MYSOs in the Large Magellanic Cloud (LMC). We took advantage of the s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.02690v1-abstract-full').style.display = 'inline'; document.getElementById('2002.02690v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2002.02690v1-abstract-full" style="display: none;"> The process of massive star ($M\geq8~M_\odot$) formation is still poorly understood. Observations of massive young stellar objects (MYSOs) are challenging due to their rarity, short formation timescale, large distances, and high circumstellar extinction. Here, we present the results of a spectroscopic analysis of a population of MYSOs in the Large Magellanic Cloud (LMC). We took advantage of the spectral resolution and wavelength coverage of X-shooter (300-2500 nm), mounted on the European Southern Observatory Very Large Telescope, to detect characteristic spectral features in a dozen MYSO candidates near 30 Doradus, the largest starburst region in the Local Group hosting the most massive stars known. The X-shooter spectra are strongly contaminated by nebular emission. We used a scaling method to subtract the nebular contamination from our objects. We detect H$伪,尾$, [O I] 630.0 nm, Ca II infrared triplet, [Fe II] 1643.5 nm, fluorescent Fe II 1687.8 nm, H$_2$ 2121.8 nm, Br$纬$, and CO bandhead emission in the spectra of multiple candidates. This leads to the spectroscopic confirmation of 10 candidates as bona fide MYSOs. We compare our observations with photometric observations from the literature and find all MYSOs to have a strong near-infrared excess. We compute lower limits to the brightness and luminosity of the MYSO candidates, confirming the near-infrared excess and the massive nature of the objects. No clear correlation is seen between the Br$纬$ luminosity and metallicity. Combining our sample with other LMC samples results in a combined detection rate of disk features such as fluorescent Fe II and CO bandheads which is consistent with the Galactic rate (40\%). Most of our MYSOs show outflow features. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.02690v1-abstract-full').style.display = 'none'; document.getElementById('2002.02690v1-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 February, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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 to A&A, 26 pages, 19 figures, 4 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 636, A54 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2001.11680">arXiv:2001.11680</a> <span> [<a href="https://arxiv.org/pdf/2001.11680">pdf</a>, <a href="https://arxiv.org/format/2001.11680">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"> A catalog of Galactic multiple systems with a red supergiant and a B star </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez%2C+M+P">M. Pantaleoni Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Negueruela%2C+I">I. Negueruela</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="2001.11680v1-abstract-short" style="display: inline;"> Binary systems composed of a red supergiant and a B star are useful probes of stellar evolution. We have searched the literature to create a catalog of 108 Galactic systems of such type, which is presented here. </span> <span class="abstract-full has-text-grey-dark mathjax" id="2001.11680v1-abstract-full" style="display: none;"> Binary systems composed of a red supergiant and a B star are useful probes of stellar evolution. We have searched the literature to create a catalog of 108 Galactic systems of such type, which is presented here. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.11680v1-abstract-full').style.display = 'none'; document.getElementById('2001.11680v1-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> 31 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">Table with 108 objects included</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> RNAAS 4 (2020) 12 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1907.01567">arXiv:1907.01567</a> <span> [<a href="https://arxiv.org/pdf/1907.01567">pdf</a>, <a href="https://arxiv.org/format/1907.01567">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="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/10.1093/mnras/stz1985">10.1093/mnras/stz1985 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Southern Photometric Local Universe Survey (S-PLUS): improved SEDs, morphologies and redshifts with 12 optical filters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=de+Oliveira%2C+C+M">C. Mendes de Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Ribeiro%2C+T">T. Ribeiro</a>, <a href="/search/astro-ph?searchtype=author&query=Schoenell%2C+W">W. Schoenell</a>, <a href="/search/astro-ph?searchtype=author&query=Kanaan%2C+A">A. Kanaan</a>, <a href="/search/astro-ph?searchtype=author&query=Overzier%2C+R+A">R. A. Overzier</a>, <a href="/search/astro-ph?searchtype=author&query=Molino%2C+A">A. Molino</a>, <a href="/search/astro-ph?searchtype=author&query=Sampedro%2C+L">L. Sampedro</a>, <a href="/search/astro-ph?searchtype=author&query=Coelho%2C+P">P. Coelho</a>, <a href="/search/astro-ph?searchtype=author&query=Barbosa%2C+C+E">C. E. Barbosa</a>, <a href="/search/astro-ph?searchtype=author&query=Cortesi%2C+A">A. Cortesi</a>, <a href="/search/astro-ph?searchtype=author&query=Costa-Duarte%2C+M+V">M. V. Costa-Duarte</a>, <a href="/search/astro-ph?searchtype=author&query=Herpich%2C+F+R">F. R. Herpich</a>, <a href="/search/astro-ph?searchtype=author&query=Hernandez-Jimenez%2C+J+A">J. A. Hernandez-Jimenez</a>, <a href="/search/astro-ph?searchtype=author&query=Placco%2C+V+M">V. M. Placco</a>, <a href="/search/astro-ph?searchtype=author&query=Xavier%2C+H+S">H. S. Xavier</a>, <a href="/search/astro-ph?searchtype=author&query=Abramo%2C+L+R">L. R. Abramo</a>, <a href="/search/astro-ph?searchtype=author&query=Saito%2C+R+K">R. K. Saito</a>, <a href="/search/astro-ph?searchtype=author&query=Chies-Santos%2C+A+L">A. L. Chies-Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Ederoclite%2C+A">A. Ederoclite</a>, <a href="/search/astro-ph?searchtype=author&query=de+Oliveira%2C+R+L">R. Lopes de Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Gon%C3%A7alves%2C+D+R">D. R. Gon莽alves</a>, <a href="/search/astro-ph?searchtype=author&query=Akras%2C+S">S. Akras</a>, <a href="/search/astro-ph?searchtype=author&query=Almeida%2C+L+A">L. A. Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Almeida-Fernandes%2C+F">F. Almeida-Fernandes</a>, <a href="/search/astro-ph?searchtype=author&query=Beers%2C+T+C">T. C. Beers</a> , et al. (120 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="1907.01567v2-abstract-short" style="display: inline;"> The Southern Photometric Local Universe Survey (S-PLUS) is imaging ~9300 deg^2 of the celestial sphere in twelve optical bands using a dedicated 0.8 m robotic telescope, the T80-South, at the Cerro Tololo Inter-American Observatory, Chile. The telescope is equipped with a 9.2k by 9.2k e2v detector with 10 um pixels, resulting in a field-of-view of 2 deg^2 with a plate scale of 0.55"/pixel. The sur… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1907.01567v2-abstract-full').style.display = 'inline'; document.getElementById('1907.01567v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1907.01567v2-abstract-full" style="display: none;"> The Southern Photometric Local Universe Survey (S-PLUS) is imaging ~9300 deg^2 of the celestial sphere in twelve optical bands using a dedicated 0.8 m robotic telescope, the T80-South, at the Cerro Tololo Inter-American Observatory, Chile. The telescope is equipped with a 9.2k by 9.2k e2v detector with 10 um pixels, resulting in a field-of-view of 2 deg^2 with a plate scale of 0.55"/pixel. The survey consists of four main subfields, which include two non-contiguous fields at high Galactic latitudes (8000 deg^2 at |b| > 30 deg) and two areas of the Galactic plane and bulge (for an additional 1300 deg^2). S-PLUS uses the Javalambre 12-band magnitude system, which includes the 5 u, g, r, i, z broad-band filters and 7 narrow-band filters centered on prominent stellar spectral features: the Balmer jump/[OII], Ca H+K, H-delta, G-band, Mg b triplet, H-alpha, and the Ca triplet. S-PLUS delivers accurate photometric redshifts (delta_z/(1+z) = 0.02 or better) for galaxies with r < 20 AB mag and redshift < 0.5, thus producing a 3D map of the local Universe over a volume of more than 1 (Gpc/h)^3. The final S-PLUS catalogue will also enable the study of star formation and stellar populations in and around the Milky Way and nearby galaxies, as well as searches for quasars, variable sources, and low-metallicity stars. In this paper we introduce the main characteristics of the survey, illustrated with science verification data highlighting the unique capabilities of S-PLUS. We also present the first public data release of ~336 deg^2 of the Stripe-82 area, which is available at http://datalab.noao.edu/splus. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1907.01567v2-abstract-full').style.display = 'none'; document.getElementById('1907.01567v2-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 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 July, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">Updated to reflect the published version (MNRAS, 489, 241). For a short introductory video of the S-PLUS project, see https://youtu.be/yc5kHrHU9Jk - The S-PLUS Data Release 1 is available at http://datalab.noao.edu/splus</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1904.11385">arXiv:1904.11385</a> <span> [<a href="https://arxiv.org/pdf/1904.11385">pdf</a>, <a href="https://arxiv.org/format/1904.11385">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/10.1051/0004-6361/201935359">10.1051/0004-6361/201935359 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MONOS: Multiplicity Of Northern O-type Spectroscopic systems. I. Project description and spectral classifications and visual multiplicity of previously known objects </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A1ez%2C+E+T">E. Trigueros P谩ez</a>, <a href="/search/astro-ph?searchtype=author&query=Negueruela%2C+I">I. Negueruela</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/astro-ph?searchtype=author&query=Lorenzo%2C+J">J. Lorenzo</a>, <a href="/search/astro-ph?searchtype=author&query=Sota%2C+A">A. Sota</a>, <a href="/search/astro-ph?searchtype=author&query=Gamen%2C+R+C">R. C. Gamen</a>, <a href="/search/astro-ph?searchtype=author&query=Fari%C3%B1a%2C+C">C. Fari帽a</a>, <a href="/search/astro-ph?searchtype=author&query=Salas%2C+J">J. Salas</a>, <a href="/search/astro-ph?searchtype=author&query=Caballero%2C+J+A">J. A. Caballero</a>, <a href="/search/astro-ph?searchtype=author&query=Morrell%2C+N+I">N. I. Morrell</a>, <a href="/search/astro-ph?searchtype=author&query=Pellerin%2C+A">A. Pellerin</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">E. J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Herrero%2C+A">A. Herrero</a>, <a href="/search/astro-ph?searchtype=author&query=Arias%2C+J+I">J. I. Arias</a>, <a href="/search/astro-ph?searchtype=author&query=Marco%2C+A">A. Marco</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="1904.11385v1-abstract-short" style="display: inline;"> [ABRIDGED] AIMS. MONOS is collecting information and studying O-type spectroscopic binaries with delta > -20 deg. In this 1st paper we describe the sample and provide spectral classifications and additional information for objects with previous SB or EB orbits. In the future we will test the validity of previous solutions and calculate new SB orbits. METHODS.The spectra in this paper have 2 source… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.11385v1-abstract-full').style.display = 'inline'; document.getElementById('1904.11385v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1904.11385v1-abstract-full" style="display: none;"> [ABRIDGED] AIMS. MONOS is collecting information and studying O-type spectroscopic binaries with delta > -20 deg. In this 1st paper we describe the sample and provide spectral classifications and additional information for objects with previous SB or EB orbits. In the future we will test the validity of previous solutions and calculate new SB orbits. METHODS.The spectra in this paper have 2 sources: GOSSS, which is obtaining blue-violet R~2500 spectroscopy of thousands of massive stars, and LiLiMaRlin, a library of libraries of high-resolution spectroscopy of massive stars obtained from 4 different surveys and additional data from our own observing programs and public archives. We also use lucky images from AstraLux. RESULTS. We present homogeneous spectral classifications for 92 O-type spectroscopic multiple systems and 10 optical companions. We discuss the visual multiplicity of each system with the support of AstraLux images and additional sources. For 11 O-type objects and for 6 B-type objects we present their first GOSSS spectral classifications. For 2 known EBs we detect SB2/SB1 lines for the first time, to which we add a third system already reported by us recently. For 2 previous SB1 systems we detect their SB2 nature for the first time and give their first separate spectral classifications, something we also do for a 3rd object just recently identified as a SB2. We also detect 9 new astrometric companions and provide updated information on several others. For sigma Ori AaAbB we provide spectral classifications for the 3 components with a single observation for the first time thanks to a lucky spectroscopy observation obtained close to the Aa,Ab periastron and for theta^1 Ori CaCb we add it to the class of Galactic Of?p stars, raising the number of its members to 6. Our sample of O-type spectroscopic binaries contains more triple/higher-order systems than double systems. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.11385v1-abstract-full').style.display = 'none'; document.getElementById('1904.11385v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">36 pages, accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 626, A20 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1904.01577">arXiv:1904.01577</a> <span> [<a href="https://arxiv.org/pdf/1904.01577">pdf</a>, <a href="https://arxiv.org/format/1904.01577">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/10.1093/mnras/stz842">10.1093/mnras/stz842 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The GALANTE Photometric System </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lorenzo-Guti%C3%A9rrez%2C+A">A. Lorenzo-Guti茅rrez</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">E. J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Mar%C3%ADn-Franch%2C+A">A. Mar铆n-Franch</a>, <a href="/search/astro-ph?searchtype=author&query=Ederoclite%2C+A">A. Ederoclite</a>, <a href="/search/astro-ph?searchtype=author&query=Crist%C3%B3bal-Hornillos%2C+D">D. Crist贸bal-Hornillos</a>, <a href="/search/astro-ph?searchtype=author&query=Varela%2C+J">J. Varela</a>, <a href="/search/astro-ph?searchtype=author&query=Rami%C3%B3%2C+H+V">H. V谩zquez Rami贸</a>, <a href="/search/astro-ph?searchtype=author&query=Cenarro%2C+J">J. Cenarro</a>, <a href="/search/astro-ph?searchtype=author&query=Lennon%2C+D+J">D. J. Lennon</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Lario%2C+P">P. Garc铆a-Lario</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="1904.01577v1-abstract-short" style="display: inline;"> This paper describes the characterization of the GALANTE photometric system, a seven intermediate- and narrow-band filter system with a wavelength coverage from 3000 $脜$ to 9000 $脜$ . We describe the photometric system presenting the full sensitivity curve as a product of the filter sensitivity, CCD, telescope mirror, and atmospheric transmission curves, as well as some first- and second-order mom… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.01577v1-abstract-full').style.display = 'inline'; document.getElementById('1904.01577v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1904.01577v1-abstract-full" style="display: none;"> This paper describes the characterization of the GALANTE photometric system, a seven intermediate- and narrow-band filter system with a wavelength coverage from 3000 $脜$ to 9000 $脜$ . We describe the photometric system presenting the full sensitivity curve as a product of the filter sensitivity, CCD, telescope mirror, and atmospheric transmission curves, as well as some first- and second-order moments of this sensitivity function. The GALANTE photometric system is composed of four filters from the J-PLUS photometric system, a twelve broad-to-narrow filter system, and three exclusive filters, specifically designed to measure the physical parameters of stars such as effective temperature $T_{\rm eff}$, $\log(g)$, metallicity, colour excess $E(4405-5495)$, and extinction type $R_{5495}$. Two libraries, the Next Generation Spectral Library (NGSL) and the one presented in Ma铆z Apell谩niz & Weiler (2018), have been used to determine the transformation equations between the Sloan Digital Sky Survey ($\textit{SDSS}$) $\textit{ugriz}$ photometry and the GALANTE photometric system. We will use this transformation to calibrate the zero points of GALANTE images. To this end, a preliminary photometric calibration of GALANTE has been made based on two different $\textit{griz}$ libraries ($\textit{SDSS}$ DR12 and ATLAS All-Sky Stellar Reference Catalog, hereinafter $\textit{RefCat2}$). A comparison between both zero points is performed leading us to the choice of $\textit{RefCat2}$ as the base catalogue for this calibration, and applied to a field in the Cyg OB2 association. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.01577v1-abstract-full').style.display = 'none'; document.getElementById('1904.01577v1-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 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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 in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1812.10861">arXiv:1812.10861</a> <span> [<a href="https://arxiv.org/pdf/1812.10861">pdf</a>, <a href="https://arxiv.org/format/1812.10861">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/10.1093/mnras/stz005">10.1093/mnras/stz005 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Spectroscopic study of the extremely young O-type triple system Herschel 36 A in the Hourglass Nebula. I. Orbital properties </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Campillay%2C+A+R">Abdo R. Campillay</a>, <a href="/search/astro-ph?searchtype=author&query=Arias%2C+J+I">Julia I. Arias</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">Rodolfo H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Morrell%2C+N+I">Nidia I. Morrell</a>, <a href="/search/astro-ph?searchtype=author&query=Gamen%2C+R+C">Roberto C. Gamen</a>, <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">Jes煤s Ma铆z Apell谩niz</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="1812.10861v1-abstract-short" style="display: inline;"> We present a detailed spectroscopic study of Herschel 36 A (H36A), the main stellar component of the massive multiple system Herschel 36 in the Hourglass Nebula, based on high-resolution optical spectra obtained along an 11 years span. The three stellar components present in the spectrum of H36A are separated by means of a spectral disentangling technique. Individual spectral classifications are i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.10861v1-abstract-full').style.display = 'inline'; document.getElementById('1812.10861v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1812.10861v1-abstract-full" style="display: none;"> We present a detailed spectroscopic study of Herschel 36 A (H36A), the main stellar component of the massive multiple system Herschel 36 in the Hourglass Nebula, based on high-resolution optical spectra obtained along an 11 years span. The three stellar components present in the spectrum of H36A are separated by means of a spectral disentangling technique. Individual spectral classifications are improved, and high precision orbital solutions for the inner and the outer orbits are calculated. H36A is confirmed to be a hierarchical triple system composed of a close massive binary (Ab1+Ab2, O9.5 V+B0.7 V) in wide orbit around a third O-type star (Aa, O7.5 Vz). The inner-pair orbit is characterized by a period of 1.54157 +/- 0.00006 days, and semi-amplitudes of 181.2 +/- 0.7 and 295.4 +/- 1.7 km/s. The outer orbit has a period of 492.81 +/- 0.69 days, and semi-amplitudes of 62.0 +/- 0.6 and 42.4 +/- 0.8 km/s. Inner and outer orbits are not coplanar, having a relative inclination of at least 20 degrees. Dynamical minimum masses of 20.6 +/- 0.8 Msun, 18.7 +/- 1.1 Msun, and 11.5 +/- 1.1 Msun are derived for the Aa, Ab1, and Ab2 components, respectively, in reasonable agreement with the theoretical calibrations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.10861v1-abstract-full').style.display = 'none'; document.getElementById('1812.10861v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 December, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Paper accepted in the Monthly Notices of the Royal Astronomical Society</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1812.04999">arXiv:1812.04999</a> <span> [<a href="https://arxiv.org/pdf/1812.04999">pdf</a>, <a href="https://arxiv.org/format/1812.04999">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/10.3847/2041-8213/aaf811">10.3847/2041-8213/aaf811 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Sequoia in the Garden: FSR 1758 - Dwarf Galaxy or Giant Globular Cluster? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Barba%2C+R+H">R. H. Barba</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Geisler%2C+D">D. Geisler</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso-Garcia%2C+J">J. Alonso-Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Hempel%2C+M">M. Hempel</a>, <a href="/search/astro-ph?searchtype=author&query=Monachesi%2C+A">A. Monachesi</a>, <a href="/search/astro-ph?searchtype=author&query=Arias%2C+J+I">J. I. Arias</a>, <a href="/search/astro-ph?searchtype=author&query=Gomez%2C+F+A">F. A. Gomez</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="1812.04999v1-abstract-short" style="display: inline;"> We present the physical characterization of FSR 1758, a new large, massive object very recently discovered in the Galactic Bulge. The combination of optical data from the 2nd Gaia Data Release (GDR2) and the DECam Plane Survey (DECaPS), and near-IR data from the VISTA Variables in the V铆a L谩ctea Extended Survey (VVVX) led to a clean sample of likely members. Based on this integrated dataset, posit… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.04999v1-abstract-full').style.display = 'inline'; document.getElementById('1812.04999v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1812.04999v1-abstract-full" style="display: none;"> We present the physical characterization of FSR 1758, a new large, massive object very recently discovered in the Galactic Bulge. The combination of optical data from the 2nd Gaia Data Release (GDR2) and the DECam Plane Survey (DECaPS), and near-IR data from the VISTA Variables in the V铆a L谩ctea Extended Survey (VVVX) led to a clean sample of likely members. Based on this integrated dataset, position, distance, reddening, size, metallicity, absolute magnitude, and proper motion of this object are measured. We estimate the following parameters: $伪=17:31:12$, $未=-39:48:30$ (J2000), $D=11.5 \pm 1.0$ kpc, $E(J-Ks)=0.20 \pm 0.03$ mag, $R_c=10$ pc, $R_t=150$ pc, $[Fe/H]=-1.5 \pm 0.3$ dex, $M_i < -8.6 \pm 1.0$, $渭_伪 = -2.85$ mas yr$^{-1}$, and $渭_未 = 2.55$ mas yr$^{-1}$. The nature of this object is discussed. If FRS 1758 is a genuine globular cluster, it is one of the largest in the Milky Way, with a size comparable or even larger than that of $蠅$ Cen, being also an extreme outlier in the size vs. Galactocentric distance diagram. The presence of a concentration of long-period RR Lyrae variable stars and blue horizontal branch stars suggests that it is a typical metal-poor globular cluster of Oosterhoff type II. Further exploration of a larger surrounding field reveals common proper motion stars, suggesting either tidal debris or that FRS\,1758 is actually the central part of a larger extended structure such as a new dwarf galaxy, tentatively named as Scorpius. In either case, this object is remarkable, and its discovery graphically illustrates the possibility to find other large objects hidden in the Galactic Bulge using future surveys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.04999v1-abstract-full').style.display = 'none'; document.getElementById('1812.04999v1-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 December, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted Astrophysical Journal Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1811.10113">arXiv:1811.10113</a> <span> [<a href="https://arxiv.org/pdf/1811.10113">pdf</a>, <a href="https://arxiv.org/format/1811.10113">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/10.1093/mnras/sty3227">10.1093/mnras/sty3227 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Extreme resonance line profile variations in the ultraviolet spectra of NGC 1624-2: probing the giant magnetosphere of the most strongly magnetized known O-type star </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=David-Uraz%2C+A">A. David-Uraz</a>, <a href="/search/astro-ph?searchtype=author&query=Erba%2C+C">C. Erba</a>, <a href="/search/astro-ph?searchtype=author&query=Petit%2C+V">V. Petit</a>, <a href="/search/astro-ph?searchtype=author&query=Fullerton%2C+A+W">A. W. Fullerton</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+F">F. Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Walborn%2C+N+R">N. R. Walborn</a>, <a href="/search/astro-ph?searchtype=author&query=MacInnis%2C+R">R. MacInnis</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+D+H">D. H. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/astro-ph?searchtype=author&query=Naz%C3%A9%2C+Y">Y. Naz茅</a>, <a href="/search/astro-ph?searchtype=author&query=Owocki%2C+S+P">S. P. Owocki</a>, <a href="/search/astro-ph?searchtype=author&query=Sundqvist%2C+J+O">J. O. Sundqvist</a>, <a href="/search/astro-ph?searchtype=author&query=ud-Doula%2C+A">A. ud-Doula</a>, <a href="/search/astro-ph?searchtype=author&query=Wade%2C+G+A">G. A. Wade</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="1811.10113v1-abstract-short" style="display: inline;"> In this paper, we present high-resolution HST/COS observations of the extreme magnetic O star NGC 1624-2. These represent the first ultraviolet spectra of this archetypal object. We examine the variability of its wind-sensitive resonance lines, comparing it to that of other known magnetic O stars. In particular, the observed variations in the profiles of the CIV and SiIV doublets between low state… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.10113v1-abstract-full').style.display = 'inline'; document.getElementById('1811.10113v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1811.10113v1-abstract-full" style="display: none;"> In this paper, we present high-resolution HST/COS observations of the extreme magnetic O star NGC 1624-2. These represent the first ultraviolet spectra of this archetypal object. We examine the variability of its wind-sensitive resonance lines, comparing it to that of other known magnetic O stars. In particular, the observed variations in the profiles of the CIV and SiIV doublets between low state and high state are the largest observed in any magnetic O-type star, consistent with the expected properties of NGC 1624-2's magnetosphere. We also observe a redshifted absorption component in the low state, a feature not seen in most stars. We present preliminary modelling efforts based on the Analytic Dynamical Magnetosphere (ADM) formalism, demonstrating the necessity of using non-spherically symmetric models to determine wind/magnetospheric properties of magnetic O stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.10113v1-abstract-full').style.display = 'none'; document.getElementById('1811.10113v1-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 November, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 6 figures, accepted for publication by MNRAS (23 November 2018)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> MNRAS, 483, 2814 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1810.12192">arXiv:1810.12192</a> <span> [<a href="https://arxiv.org/pdf/1810.12192">pdf</a>, <a href="https://arxiv.org/format/1810.12192">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> GALANTE: finding all the optically accessible Galactic O+B+WR stars in the Galactic Plane </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">E. J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Lorenzo%2C+A">A. Lorenzo</a>, <a href="/search/astro-ph?searchtype=author&query=Mar%C3%ADn-Franch%2C+A">A. Mar铆n-Franch</a>, <a href="/search/astro-ph?searchtype=author&query=Ederoclite%2C+A">A. Ederoclite</a>, <a href="/search/astro-ph?searchtype=author&query=Varela%2C+J">J. Varela</a>, <a href="/search/astro-ph?searchtype=author&query=Rami%C3%B3%2C+H+V">H. V谩zquez Rami贸</a>, <a href="/search/astro-ph?searchtype=author&query=Cenarro%2C+J">J. Cenarro</a>, <a href="/search/astro-ph?searchtype=author&query=Lennon%2C+D+J">D. J. Lennon</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Lario%2C+P">P. Garc铆a-Lario</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1810.12192v1-abstract-short" style="display: inline;"> GALANTE is an optical photometric survey with seven intermediate/narrow filters that has been covering the Galactic Plane since 2016 using the Javalambre T80 and Cerro Tololo T80S telescopes. The P.I.s of the northern part (GALANTE NORTE) are Emilio J. Alfaro and Jes煤s Ma铆z Apell谩niz. and the P.I. of the southern part (GALANTE SUR) is Rodolfo H. Barb谩. The detector has a continuous 1.4 degr x 1.4… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1810.12192v1-abstract-full').style.display = 'inline'; document.getElementById('1810.12192v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1810.12192v1-abstract-full" style="display: none;"> GALANTE is an optical photometric survey with seven intermediate/narrow filters that has been covering the Galactic Plane since 2016 using the Javalambre T80 and Cerro Tololo T80S telescopes. The P.I.s of the northern part (GALANTE NORTE) are Emilio J. Alfaro and Jes煤s Ma铆z Apell谩niz. and the P.I. of the southern part (GALANTE SUR) is Rodolfo H. Barb谩. The detector has a continuous 1.4 degr x 1.4 degr field of view with a sampling of 0.55"/pixel and the seven filters are optimized to detect obscured early-type stars. The survey includes long, intermediate, short, and ultrashort exposure times to reach a dynamical range close to 20 magnitudes, something never achieved for such an optical project before. The characteristics of GALANTE allow for a new type of calibration scheme using external Gaia, Tycho-2, and 2MASS data that has already led to a reanalysis of the sensitivity of the Gaia G filter. We describe the project and present some early results. GALANTE will identify the majority of the early-type massive stars within several kpc of the Sun and measure their amount and type of extinction. It will also map the Halpha nebular emission, identify emission-line stars, and do other studies of low- and intermediate-mass stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1810.12192v1-abstract-full').style.display = 'none'; document.getElementById('1810.12192v1-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 October, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">To appear in Highlights on Spanish Astrophysics X, Proceedings of the XIII Scientific Meeting of the Spanish Astronomical Society held on July 16-20, 2018, in Salamanca, Spain</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1810.10953">arXiv:1810.10953</a> <span> [<a href="https://arxiv.org/pdf/1810.10953">pdf</a>, <a href="https://arxiv.org/format/1810.10953">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> <p class="title is-5 mathjax"> The Gaia photometric calibration and results on Galactic runaways </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez%2C+M+P">M. Pantaleoni Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Lennon%2C+D+J">D. J. Lennon</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Weiler%2C+M">M. Weiler</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1810.10953v1-abstract-short" style="display: inline;"> We present results on two different Gaia-related topics. First, we describe our efforts to calibrate the three Gaia photometric passbands G, G_BP, and G_RP. We have built a new spectrophotometric HST/STIS library and used it to derive new sensitivity curves and zero points for the three bands, including recipes on how to correct some cases. Second, we present our results on Galactic runaway stars… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1810.10953v1-abstract-full').style.display = 'inline'; document.getElementById('1810.10953v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1810.10953v1-abstract-full" style="display: none;"> We present results on two different Gaia-related topics. First, we describe our efforts to calibrate the three Gaia photometric passbands G, G_BP, and G_RP. We have built a new spectrophotometric HST/STIS library and used it to derive new sensitivity curves and zero points for the three bands, including recipes on how to correct some cases. Second, we present our results on Galactic runaway stars using Gaia DR1 proper motions: we detect 76 runaway stars, 17 (possibly 19) of them not previously identified as such. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1810.10953v1-abstract-full').style.display = 'none'; document.getElementById('1810.10953v1-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 October, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">To appear in Highlights on Spanish Astrophysics X, Proceedings of the XIII Scientific Meeting of the Spanish Astronomical Society held on July 16-20, 2018, in Salamanca, Spain</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1810.10943">arXiv:1810.10943</a> <span> [<a href="https://arxiv.org/pdf/1810.10943">pdf</a>, <a href="https://arxiv.org/format/1810.10943">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"> LiLiMaRlin, a Library of Libraries of Massive-Star High-Resolution Spectra with applications to OWN, MONOS, and CollDIBs </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A1ez%2C+E+T">E. Trigueros P谩ez</a>, <a href="/search/astro-ph?searchtype=author&query=Mart%C3%ADnez%2C+I+J">I. Jim茅nez Mart铆nez</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/astro-ph?searchtype=author&query=Pellerin%2C+A">A. Pellerin</a>, <a href="/search/astro-ph?searchtype=author&query=Negueruela%2C+I">I. Negueruela</a>, <a href="/search/astro-ph?searchtype=author&query=Le%C3%A3o%2C+J+R+S">J. R. Souza Le茫o</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1810.10943v1-abstract-short" style="display: inline;"> LiLiMaRlin is a library of libraries of massive-star high-resolution optical spectra built by collecting data from [a] our spectroscopic surveys (OWN, IACOB. NoMaDS, and CAF脡-BEANS) and programs and [b] searches in public archives. The current version has 18 077 spectra of 1665 stars obtained with seven different telescopes (HET 9.2 m, NOT 2.56 m, CAHA 2.2 m, MPG/ESO 2.2 m, OHP 1.93 m, Mercator 1.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1810.10943v1-abstract-full').style.display = 'inline'; document.getElementById('1810.10943v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1810.10943v1-abstract-full" style="display: none;"> LiLiMaRlin is a library of libraries of massive-star high-resolution optical spectra built by collecting data from [a] our spectroscopic surveys (OWN, IACOB. NoMaDS, and CAF脡-BEANS) and programs and [b] searches in public archives. The current version has 18 077 spectra of 1665 stars obtained with seven different telescopes (HET 9.2 m, NOT 2.56 m, CAHA 2.2 m, MPG/ESO 2.2 m, OHP 1.93 m, Mercator 1.2 m, and Stella 1.2 m). All the spectra have been filtered to eliminate misidentifications and bad-quality ones, uniformly reprocessed, and placed on a common format. We present applications of this library of libraries to the analysis of spectroscopic binaries (OWN and MONOS, see poster by E. Trigueros P谩ez at this meeting) and the study of the interstellar medium (CollDIBs). We discuss our plans for the future. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1810.10943v1-abstract-full').style.display = 'none'; document.getElementById('1810.10943v1-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 October, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">To appear in Highlights on Spanish Astrophysics X, Proceedings of the XIII Scientific Meeting of the Spanish Astronomical Society held on July 16-20, 2018, in Salamanca, Spain</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1810.02154">arXiv:1810.02154</a> <span> [<a href="https://arxiv.org/pdf/1810.02154">pdf</a>, <a href="https://arxiv.org/ps/1810.02154">ps</a>, <a href="https://arxiv.org/format/1810.02154">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/10.1051/0004-6361/201833574">10.1051/0004-6361/201833574 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Non-synchronous rotations in massive binary systems. HD93343 revisited </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Putkuri%2C+C">C. Putkuri</a>, <a href="/search/astro-ph?searchtype=author&query=Gamen%2C+R">R. Gamen</a>, <a href="/search/astro-ph?searchtype=author&query=Morrell%2C+N+I">N. I. Morrell</a>, <a href="/search/astro-ph?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrero%2C+G+A">G. A. Ferrero</a>, <a href="/search/astro-ph?searchtype=author&query=Arias%2C+J+I">J. I. Arias</a>, <a href="/search/astro-ph?searchtype=author&query=Solivella%2C+G">G. Solivella</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1810.02154v1-abstract-short" style="display: inline;"> Context. Most massive stars are in binary or multiple systems. Several massive stars have been detected as doublelined spectroscopic binaries and among these, the OWN Survey has detected a non-negligible number whose components show very different spectral line broadening (i.e., projected rotational velocities). This fact raises a discussion about the contributing processes, such as angular-moment… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1810.02154v1-abstract-full').style.display = 'inline'; document.getElementById('1810.02154v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1810.02154v1-abstract-full" style="display: none;"> Context. Most massive stars are in binary or multiple systems. Several massive stars have been detected as doublelined spectroscopic binaries and among these, the OWN Survey has detected a non-negligible number whose components show very different spectral line broadening (i.e., projected rotational velocities). This fact raises a discussion about the contributing processes, such as angular-momentum transfer and tidal forces. Aims. We seek to constrain the physical and evolutionary status of one of such systems, the O+O binary HD 93343. Methods. We analyzed a series of high-resolution multiepoch optical spectra to determine the orbital parameters, projected rotational velocities, and evolutionary status of the system. Results. HD 93343 is a binary system comprised of two O7.5 Vz stars that each have minimum masses of approximately 22 Mo in a wide and eccentric orbit (e = 0.398$\pm$0.004; P=50.432$\pm$0.001 d). Both stars have very similar stellar parameters, and hence ages. As expected from the qualitative appearance of the combined spectrum of the system, however, these stars have very different projected rotational velocities (~65 and ~325 km/s, respectively). Conclusions. The orbits and stellar parameters obtained for both components seem to indicate that their youth and relative separation is enough to discard the effects of mass transfer and tidal friction. Thus, non-synchronization should be intrinsic to their formation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1810.02154v1-abstract-full').style.display = 'none'; document.getElementById('1810.02154v1-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, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 7 figures. Accepted to Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 618, A174 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1804.06915">arXiv:1804.06915</a> <span> [<a href="https://arxiv.org/pdf/1804.06915">pdf</a>, <a href="https://arxiv.org/format/1804.06915">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/10.1051/0004-6361/201832787">10.1051/0004-6361/201832787 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A search for Galactic runaway stars using Gaia Data Release 1 and Hipparcos proper motions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez%2C+M+P">M. Pantaleoni Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/astro-ph?searchtype=author&query=Negueruela%2C+I">I. Negueruela</a>, <a href="/search/astro-ph?searchtype=author&query=Lennon%2C+D+J">D. J. Lennon</a>, <a href="/search/astro-ph?searchtype=author&query=Sota%2C+A">A. Sota</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A1ez%2C+E+T">E. Trigueros P谩ez</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="1804.06915v2-abstract-short" style="display: inline;"> CONTEXT.The first Gaia Data Release (DR1) significantly improved the previously available proper motions for the majority of the Tycho-2 stars. AIMS. We want to detect runaway stars using Gaia DR1 proper motions and compare our results with previous searches. METHODS. Runaway O stars and BA supergiants are detected using a 2-D proper-motion method. The sample is selected using Simbad, spectra from… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.06915v2-abstract-full').style.display = 'inline'; document.getElementById('1804.06915v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1804.06915v2-abstract-full" style="display: none;"> CONTEXT.The first Gaia Data Release (DR1) significantly improved the previously available proper motions for the majority of the Tycho-2 stars. AIMS. We want to detect runaway stars using Gaia DR1 proper motions and compare our results with previous searches. METHODS. Runaway O stars and BA supergiants are detected using a 2-D proper-motion method. The sample is selected using Simbad, spectra from our GOSSS project, literature spectral types, and photometry processed using CHORIZOS. RESULTS. We detect 76 runaway stars, 17 (possibly 19) of them with no prior identification as such, with an estimated detection rate of approximately one half of the real runaway fraction. An age effect appears to be present, with objects of spectral subtype B1 and later having travelled for longer distances than runaways of earlier subtypes. We also tentatively propose that the fraction of runaways is lower among BA supergiants that among O stars but further studies using future Gaia data releases are needed to confirm this. The frequency of fast rotators is high among runaway O stars, which indicates that a significant fraction of them (and possibly a majority) is produced in supernova explosions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.06915v2-abstract-full').style.display = 'none'; document.getElementById('1804.06915v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 April, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 April, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">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 616, A149 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1804.03133">arXiv:1804.03133</a> <span> [<a href="https://arxiv.org/pdf/1804.03133">pdf</a>, <a href="https://arxiv.org/format/1804.03133">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201832885">10.1051/0004-6361/201832885 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Lucky Spectroscopy, an equivalent technique to Lucky Imaging. Spatially resolved spectroscopy of massive close visual binaries using the William Herschel Telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/astro-ph?searchtype=author&query=Sota%2C+A">A. Sota</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A1ez%2C+E+T">E. Trigueros P谩ez</a>, <a href="/search/astro-ph?searchtype=author&query=Caballero%2C+J+A">J. A. Caballero</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">E. J. Alfaro</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="1804.03133v1-abstract-short" style="display: inline;"> CONTEXT: Many massive stars have nearby companions whose presence hamper their characterization through spectroscopy. AIMS: We want to obtain spatially resolved spectroscopy of close massive visual binaries to derive their spectral types. METHODS: We obtain a large number of short long-slit spectroscopic exposures of five close binaries under good seeing conditions, select those with the best char… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.03133v1-abstract-full').style.display = 'inline'; document.getElementById('1804.03133v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1804.03133v1-abstract-full" style="display: none;"> CONTEXT: Many massive stars have nearby companions whose presence hamper their characterization through spectroscopy. AIMS: We want to obtain spatially resolved spectroscopy of close massive visual binaries to derive their spectral types. METHODS: We obtain a large number of short long-slit spectroscopic exposures of five close binaries under good seeing conditions, select those with the best characteristics, extract the spectra using multiple-profile fitting, and combine the results to derive spatially separated spectra. RESULTS: We demonstrate the usefulness of Lucky Spectroscopy by presenting the spatially resolved spectra of the components of each system, in two cases with separations of only ~0.3". Those are delta Ori Aa+Ab (resolved in the optical for the first time) and sigma Ori AaAb+B (first time ever resolved). We also spatially resolve 15 Mon AaAb+B, zeta Ori AaAb+B (both previously resolved with GOSSS, the Galactic O-Star Spectroscopic Survey), and eta Ori AaAb+B, a system with two spectroscopic B+B binaries and a fifth visual component. The systems have in common that they are composed of an inner pair of slow rotators orbited by one or more fast rotators, a characteristic that could have consequences for the theories of massive star formation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.03133v1-abstract-full').style.display = 'none'; document.getElementById('1804.03133v1-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 April, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A, 7 pages</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 615, A161 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1803.10833">arXiv:1803.10833</a> <span> [<a href="https://arxiv.org/pdf/1803.10833">pdf</a>, <a href="https://arxiv.org/format/1803.10833">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/10.1051/0004-6361/201730487">10.1051/0004-6361/201730487 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Massive young stellar objects in the N66/NGC346 region of the SMC </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rubio%2C+M">Monica Rubio</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">Rodolfo H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Kalari%2C+V+M">Venu M. Kalari</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="1803.10833v1-abstract-short" style="display: inline;"> We present HK spectra of three sources located in the N66 region of the Small Magellanic Cloud. The sources display prominent stellar Br Gamma and extended H2 emission, and exhibit infrared excesses at lambda > 2 micron. Based on their spectral features, and photometric spectral energy distributions, we suggest that these sources are massive young stellar objects (mYSOs). The findings are interpre… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1803.10833v1-abstract-full').style.display = 'inline'; document.getElementById('1803.10833v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1803.10833v1-abstract-full" style="display: none;"> We present HK spectra of three sources located in the N66 region of the Small Magellanic Cloud. The sources display prominent stellar Br Gamma and extended H2 emission, and exhibit infrared excesses at lambda > 2 micron. Based on their spectral features, and photometric spectral energy distributions, we suggest that these sources are massive young stellar objects (mYSOs). The findings are interpreted as evidence of on-going high mass star formation in N66. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1803.10833v1-abstract-full').style.display = 'none'; document.getElementById('1803.10833v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 March, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication on Astronomy and Astrophysics Journal, acceptance date 21/03/2018 (includes 12 pages, 5 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/1712.09759">arXiv:1712.09759</a> <span> [<a href="https://arxiv.org/pdf/1712.09759">pdf</a>, <a href="https://arxiv.org/ps/1712.09759">ps</a>, <a href="https://arxiv.org/format/1712.09759">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/10.1051/0004-6361/201731723">10.1051/0004-6361/201731723 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Resolving the clumpy circumstellar environment of the B[e] supergiant LHA 120-S 35 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Torres%2C+A+F">Andrea F. Torres</a>, <a href="/search/astro-ph?searchtype=author&query=Cidale%2C+L+S">Lydia S. Cidale</a>, <a href="/search/astro-ph?searchtype=author&query=Kraus%2C+M">Michaela Kraus</a>, <a href="/search/astro-ph?searchtype=author&query=Arias%2C+M+L">Mar铆a L. Arias</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">Rodolfo H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Maravelias%2C+G">Grigoris Maravelias</a>, <a href="/search/astro-ph?searchtype=author&query=Fernandes%2C+M+B">Marcelo Borges Fernandes</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="1712.09759v1-abstract-short" style="display: inline;"> B[e] supergiants (SGs) are massive post-main-sequence stars, surrounded by a complex circumstellar (CS) environment. The aim of this work is to investigate the structure and kinematics of the CS disc of the B[e] SG LHA 120-S 35. We used high-resolution optical spectra obtained in different years to model the forbidden emission lines and determine the kinematical properties of their line-forming re… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1712.09759v1-abstract-full').style.display = 'inline'; document.getElementById('1712.09759v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1712.09759v1-abstract-full" style="display: none;"> B[e] supergiants (SGs) are massive post-main-sequence stars, surrounded by a complex circumstellar (CS) environment. The aim of this work is to investigate the structure and kinematics of the CS disc of the B[e] SG LHA 120-S 35. We used high-resolution optical spectra obtained in different years to model the forbidden emission lines and determine the kinematical properties of their line-forming regions, assuming Keplerian rotation. We also used low-resolution near-infrared (IR) spectra to explore the variability of molecular emission. LHA 120-S 35 displays spectral variability in both optical and IR regions. The P-Cygni line profiles of H I, as well as those of Fe II and O I, suggest the presence of a strong bipolar clumped wind. We distinguish density enhancements in the P-Cygni absorption component of the first Balmer lines, which show variations in both velocity and strength. The P-Cygni profile emission component is double-peaked, indicating the presence of a rotating CS disc. We also observe line-profile variations in the permitted and forbidden features of Fe II and O I. In the IR, we detect variations in the intensity of the H I emission lines as well as in the emission of the CO band-heads. Moreover, we find that the profiles of each [Ca II] and [O I] emission lines contain contributions from spatially different (complete or partial) rings. Globally, we find evidence of detached multi-ring structures, revealing density variations along the disc. We suggest that LHA 120-S 35 has passed through the red-supergiant (RSG) phase and evolves back bluewards in the Hertzsprung-Russell diagram. The formation of the complex CS structure could be the result of the wind-wind interactions of the post-RSG wind with the previously ejected material from the RSG. However, the presence of a binary companion can not be excluded. Finally, we find that LHA 120-S 35 belongs to a young stellar cluster. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1712.09759v1-abstract-full').style.display = 'none'; document.getElementById('1712.09759v1-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 December, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 23 figures, accepted to Astronomy and Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 612, A113 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1712.09228">arXiv:1712.09228</a> <span> [<a href="https://arxiv.org/pdf/1712.09228">pdf</a>, <a href="https://arxiv.org/format/1712.09228">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/10.1051/0004-6361/201732050">10.1051/0004-6361/201732050 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Optical-NIR dust extinction towards Galactic O stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</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="1712.09228v2-abstract-short" style="display: inline;"> [ABRIDGED] Context. O stars are excellent tracers of the intervening ISM because of their high luminosity, blue intrinsic SED, and relatively featureless spectra. We are currently conducting GOSSS, which is generating a large sample of O stars with accurate spectral types within several kpc of the Sun. Aims. To obtain a global picture of the properties of dust extinction in the solar neighborhood… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1712.09228v2-abstract-full').style.display = 'inline'; document.getElementById('1712.09228v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1712.09228v2-abstract-full" style="display: none;"> [ABRIDGED] Context. O stars are excellent tracers of the intervening ISM because of their high luminosity, blue intrinsic SED, and relatively featureless spectra. We are currently conducting GOSSS, which is generating a large sample of O stars with accurate spectral types within several kpc of the Sun. Aims. To obtain a global picture of the properties of dust extinction in the solar neighborhood based on optical-NIR photometry of O stars with accurate spectral types. Methods. We have processed a photometric set with the CHORIZOS code to measure the amount and type of extinction towards 562 O-type stellar systems. We have tested three different families of extinction laws and analyzed our results with the help of additional archival data. Results. The Ma铆z Apell谩niz et al. (2014) family of extinction laws provides a better description of Galactic dust that either the Cardelli et al. (1989) or Fitzpatrick (1999) families, so it should be preferentially used. In many cases O stars and late-type stars experience similar amounts of extinction at similar distances but some O stars are located close to the molecular clouds left over from their births and have larger extinctions than the average for nearby late-type populations. In qualitative terms, O stars experience a more diverse extinction than late-type stars, as some are affected by the small-grain-size, low-R_5495 effect of molecular clouds and others by the large-grain-size, high-R_5495 effect of H II regions. Late-type stars experience a narrower range of grain sizes or R_5495, as their extinction is predominantly caused by the average, diffuse ISM. We propose that the reason for the existence of large-grain-size, high-R_5495 regions in the ISM in the form of H II regions and hot-gas bubbles is the selective destruction of small dust grains by EUV photons and possibly by thermal sputtering by atoms or ions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1712.09228v2-abstract-full').style.display = 'none'; document.getElementById('1712.09228v2-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 December, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 December, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">33 pages, accepted for publication in A&A. This second version includes language editing, other minor changes to the text, and the solution to formatting issues in the main table</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 613, A9 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1711.10043">arXiv:1711.10043</a> <span> [<a href="https://arxiv.org/pdf/1711.10043">pdf</a>, <a href="https://arxiv.org/format/1711.10043">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/10.1051/0004-6361/201731543">10.1051/0004-6361/201731543 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The IACOB project. V. Spectroscopic parameters of the O-type stars in the modern grid of standards for spectral classification </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Holgado%2C+G">G. Holgado</a>, <a href="/search/astro-ph?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Puls%2C+J">J. Puls</a>, <a href="/search/astro-ph?searchtype=author&query=Herrero%2C+A">A. Herrero</a>, <a href="/search/astro-ph?searchtype=author&query=Castro%2C+N">N. Castro</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia%2C+M">M. Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/astro-ph?searchtype=author&query=Negueruela%2C+I">I. Negueruela</a>, <a href="/search/astro-ph?searchtype=author&query=Sab%C3%ADn-Sanjuli%C3%A1n%2C+C">C. Sab铆n-Sanjuli谩n</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="1711.10043v2-abstract-short" style="display: inline;"> The IACOB and OWN surveys are two ambitious complementary observational projects which have made available a large multi-epoch spectroscopic database of optical high resolution spectra of Galactic massive O-type stars. As a first step in the study of the full sample of (more than 350) O stars surveyed by the IACOB/OWN projects, we have performed the quantitative spectroscopic analysis of a subsamp… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1711.10043v2-abstract-full').style.display = 'inline'; document.getElementById('1711.10043v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1711.10043v2-abstract-full" style="display: none;"> The IACOB and OWN surveys are two ambitious complementary observational projects which have made available a large multi-epoch spectroscopic database of optical high resolution spectra of Galactic massive O-type stars. As a first step in the study of the full sample of (more than 350) O stars surveyed by the IACOB/OWN projects, we have performed the quantitative spectroscopic analysis of a subsample of 128 stars included in the modern grid of O-type standards for spectral classification. We use semi-automatized tools to determine the set of spectroscopic parameters that can be obtained from the optical spectrum of O-type stars. We also benefit from the multi-epoch character of the surveys to perform a spectroscopic variability study of the sample, accounting for spectroscopic binarity and variability of the main wind diagnostic lines. We provide a general overview of the stellar and wind parameters of this reference sample, and updated recipes for the SpT\,--\,Teff/log g calibrations for Galactic O-type stars. We evaluate our semi-automatized analysis strategy with $\sim$40 stars from the literature, and find a good agreement. The agreement between the synthetic spectra associated with fastwind best fitting models and the observed spectra is good for most targets, but 46 stars present a particular behavior of the wind diagnostic lines that cannot be reproduced by our grid of spherically symmetric unclumped models. These are potential targets of interest for more detailed investigations of clumpy winds and/or the existence of additional circumstellar components. Last, our variability study has led to the detection of signatures of spectroscopic binarity in 27\% of the stars and small amplitude radial velocity variations in the photospheric lines of another 30\%. Additionally, 31\% of the investigated stars show variability in the wind diagnostic lines. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1711.10043v2-abstract-full').style.display = 'none'; document.getElementById('1711.10043v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 June, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 November, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 18 figures, accepted for publication in Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 613, A65 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1711.00660">arXiv:1711.00660</a> <span> [<a href="https://arxiv.org/pdf/1711.00660">pdf</a>, <a href="https://arxiv.org/format/1711.00660">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/10.3847/1538-4357/aaa765">10.3847/1538-4357/aaa765 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Stellar Multiplicity Meets Stellar Evolution And Metallicity: The APOGEE View </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Badenes%2C+C">Carles Badenes</a>, <a href="/search/astro-ph?searchtype=author&query=Mazzola%2C+C">Christine Mazzola</a>, <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+T+A">Todd A. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Covey%2C+K">Kevin Covey</a>, <a href="/search/astro-ph?searchtype=author&query=Freeman%2C+P+E">Peter E. Freeman</a>, <a href="/search/astro-ph?searchtype=author&query=Walker%2C+M+G">Matthew G. Walker</a>, <a href="/search/astro-ph?searchtype=author&query=Moe%2C+M">Maxwell Moe</a>, <a href="/search/astro-ph?searchtype=author&query=Troup%2C+N">Nicholas Troup</a>, <a href="/search/astro-ph?searchtype=author&query=Nidever%2C+D">David Nidever</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+C+A">Carlos Allende Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Andrews%2C+B">Brett Andrews</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">Rodolfo H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Beers%2C+T+C">Timothy C. Beers</a>, <a href="/search/astro-ph?searchtype=author&query=Bovy%2C+J">Jo Bovy</a>, <a href="/search/astro-ph?searchtype=author&query=Carlberg%2C+J+K">Joleen K. Carlberg</a>, <a href="/search/astro-ph?searchtype=author&query=De+Lee%2C+N">Nathan De Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+J">Jennifer Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Lewis%2C+H">Hannah Lewis</a>, <a href="/search/astro-ph?searchtype=author&query=Majewski%2C+S+R">Steven R. Majewski</a>, <a href="/search/astro-ph?searchtype=author&query=Pinsonneault%2C+M">Marc Pinsonneault</a>, <a href="/search/astro-ph?searchtype=author&query=Sobeck%2C+J">Jennifer Sobeck</a>, <a href="/search/astro-ph?searchtype=author&query=Stassun%2C+K+G">Keivan G. Stassun</a>, <a href="/search/astro-ph?searchtype=author&query=Stringfellow%2C+G">Guy Stringfellow</a>, <a href="/search/astro-ph?searchtype=author&query=Zasowski%2C+G">Gail Zasowski</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="1711.00660v2-abstract-short" style="display: inline;"> We use the multi-epoch radial velocities acquired by the APOGEE survey to perform a large scale statistical study of stellar multiplicity for field stars in the Milky Way, spanning the evolutionary phases between the main sequence and the red clump. We show that the distribution of maximum radial velocity shifts (\drvm) for APOGEE targets is a strong function of \logg, with main sequence stars sho… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1711.00660v2-abstract-full').style.display = 'inline'; document.getElementById('1711.00660v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1711.00660v2-abstract-full" style="display: none;"> We use the multi-epoch radial velocities acquired by the APOGEE survey to perform a large scale statistical study of stellar multiplicity for field stars in the Milky Way, spanning the evolutionary phases between the main sequence and the red clump. We show that the distribution of maximum radial velocity shifts (\drvm) for APOGEE targets is a strong function of \logg, with main sequence stars showing \drvm\ as high as $\sim$300 \kms, and steadily dropping down to $\sim$30 \kms\ for \logg$\sim$0, as stars climb up the Red Giant Branch (RGB). Red clump stars show a distribution of \drvm\ values comparable to that of stars at the tip of the RGB, implying they have similar multiplicity characteristics. The observed attrition of high \drvm\ systems in the RGB is consistent with a lognormal period distribution in the main sequence and a multiplicity fraction of 0.35, which is truncated at an increasing period as stars become physically larger and undergo mass transfer after Roche Lobe Overflow during H shell burning. The \drvm\ distributions also show that the multiplicity characteristics of field stars are metallicity dependent, with metal-poor ([Fe/H]$\lesssim-0.5$) stars having a multiplicity fraction a factor 2-3 higher than metal-rich ([Fe/H]$\gtrsim0.0$) stars. This has profound implications for the formation rates of interacting binaries observed by astronomical transient surveys and gravitational wave detectors, as well as the habitability of circumbinary planets. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1711.00660v2-abstract-full').style.display = 'none'; document.getElementById('1711.00660v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 January, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 November, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 13 figures, replaced with version 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/1612.07923">arXiv:1612.07923</a> <span> [<a href="https://arxiv.org/pdf/1612.07923">pdf</a>, <a href="https://arxiv.org/ps/1612.07923">ps</a>, <a href="https://arxiv.org/format/1612.07923">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/10.1017/S1743921317001831">10.1017/S1743921317001831 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> New runaway O-type stars in the first Gaia Data Release </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Apell%C3%A1niz%2C+J+M">J. Ma铆z Apell谩niz</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/astro-ph?searchtype=author&query=Negueruela%2C+I">I. Negueruela</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A1ez%2C+E+T">E. Trigueros P谩ez</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="1612.07923v1-abstract-short" style="display: inline;"> We have detected 13 new runaway-star candidates of spectral type O combining the TGAS (Tycho-Gaia Astrometric Solution) proper motions from Gaia Data Release 1 (DR1) and the sample from GOSSS (Galactic O-Star Spectroscopic Survey). We have also combined TGAS and Hipparcos proper motions to check that our technique recovers many of the previously known O-type runaways in the sample. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1612.07923v1-abstract-full" style="display: none;"> We have detected 13 new runaway-star candidates of spectral type O combining the TGAS (Tycho-Gaia Astrometric Solution) proper motions from Gaia Data Release 1 (DR1) and the sample from GOSSS (Galactic O-Star Spectroscopic Survey). We have also combined TGAS and Hipparcos proper motions to check that our technique recovers many of the previously known O-type runaways in the sample. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1612.07923v1-abstract-full').style.display = 'none'; document.getElementById('1612.07923v1-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, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">To appear in IAUS 239, the lives and death-throes of massive stars</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1611.05223">arXiv:1611.05223</a> <span> [<a href="https://arxiv.org/pdf/1611.05223">pdf</a>, <a href="https://arxiv.org/ps/1611.05223">ps</a>, <a href="https://arxiv.org/format/1611.05223">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/10.1051/0004-6361/201629548">10.1051/0004-6361/201629548 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A study of the effect of rotational mixing on massive stars evolution: surface abundances of Galactic O7-8 giant stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Martins%2C+F">F. Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Simon-Diaz%2C+S">S. Simon-Diaz</a>, <a href="/search/astro-ph?searchtype=author&query=Barba%2C+R+H">R. H. Barba</a>, <a href="/search/astro-ph?searchtype=author&query=Gamen%2C+R+C">R. C. Gamen</a>, <a href="/search/astro-ph?searchtype=author&query=Ekstroem%2C+S">S. Ekstroem</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="1611.05223v1-abstract-short" style="display: inline;"> Massive star evolution remains only partly constrained. In particular, the exact role of rotation has been questioned by puzzling properties of OB stars in the Magellanic Clouds. Our goal is to study the relation between surface chemical composition and rotational velocity, and to test predictions of evolutionary models including rotation. We have performed a spectroscopic analysis of a sample of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.05223v1-abstract-full').style.display = 'inline'; document.getElementById('1611.05223v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1611.05223v1-abstract-full" style="display: none;"> Massive star evolution remains only partly constrained. In particular, the exact role of rotation has been questioned by puzzling properties of OB stars in the Magellanic Clouds. Our goal is to study the relation between surface chemical composition and rotational velocity, and to test predictions of evolutionary models including rotation. We have performed a spectroscopic analysis of a sample of fifteen Galactic O7-8 giant stars. This sample is homogeneous in terms of mass, metallicity and evolutionary state. It is made of stars with a wide range of projected rotational velocities. We show that the sample stars are located on the second half of the main sequence, in a relatively narrow mass range (25-40 Msun). Almost all stars with projected rotational velocities above 100 km/s have N/C ratios about ten times the initial value. Below 100 km/s a wide range of N/C values is observed. The relation between N/C and surface gravity is well reproduced by various sets of models. Some evolutionary models including rotation are also able to consistently explain slowly rotating, highly enriched stars. This is due to differential rotation which efficiently transports nucleosynthesis products and allows the surface to rotate slower than the core. In addition, angular momentum removal by winds amplifies surface braking on the main sequence. Comparison of the surface composition of O7-8 giant stars with a sample of B stars with initial masses about four times smaller reveal that chemical enrichment scales with initial mass, as expected from theory. Although evolutionary models that include rotation face difficulties in explaining the chemical properties of O- and B-type stars at low metallicity, some of them can consistently account for the properties of main-sequence Galactic O stars in the mass range 25-40 Msun <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.05223v1-abstract-full').style.display = 'none'; document.getElementById('1611.05223v1-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 November, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">14 pages, 10 figures + appendix , 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 599, A30 (2017) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1611.04502">arXiv:1611.04502</a> <span> [<a href="https://arxiv.org/pdf/1611.04502">pdf</a>, <a href="https://arxiv.org/ps/1611.04502">ps</a>, <a href="https://arxiv.org/format/1611.04502">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/10.1051/0004-6361/201628905">10.1051/0004-6361/201628905 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> B fields in OB stars (BOB): Concluding the FORS2 observing campaign </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Schoeller%2C+M">M. Schoeller</a>, <a href="/search/astro-ph?searchtype=author&query=Hubrig%2C+S">S. Hubrig</a>, <a href="/search/astro-ph?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/astro-ph?searchtype=author&query=Carroll%2C+T+A">T. A. Carroll</a>, <a href="/search/astro-ph?searchtype=author&query=Briquet%2C+M">M. Briquet</a>, <a href="/search/astro-ph?searchtype=author&query=Oskinova%2C+L+M">L. M. Oskinova</a>, <a href="/search/astro-ph?searchtype=author&query=Jarvinen%2C+S">S. Jarvinen</a>, <a href="/search/astro-ph?searchtype=author&query=Ilyin%2C+I">I. Ilyin</a>, <a href="/search/astro-ph?searchtype=author&query=Castro%2C+N">N. Castro</a>, <a href="/search/astro-ph?searchtype=author&query=Morel%2C+T">T. Morel</a>, <a href="/search/astro-ph?searchtype=author&query=Langer%2C+N">N. Langer</a>, <a href="/search/astro-ph?searchtype=author&query=Przybilla%2C+N">N. Przybilla</a>, <a href="/search/astro-ph?searchtype=author&query=Nieva%2C+M+F">M. F. Nieva</a>, <a href="/search/astro-ph?searchtype=author&query=Kholtygin%2C+A+F">A. F. Kholtygin</a>, <a href="/search/astro-ph?searchtype=author&query=Sana%2C+H">H. Sana</a>, <a href="/search/astro-ph?searchtype=author&query=Herrero%2C+A">A. Herrero</a>, <a href="/search/astro-ph?searchtype=author&query=Barba%2C+R+H">R. H. Barba</a>, <a href="/search/astro-ph?searchtype=author&query=de+Koter%2C+A">A. de Koter</a>, <a href="/search/astro-ph?searchtype=author&query=collaboration%2C+t+B">the BOB collaboration</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="1611.04502v1-abstract-short" style="display: inline;"> The "B fields in OB stars" (BOB) collaboration is based on an ESO Large Programme, to study the occurrence rate, properties, and ultimately the origin of magnetic fields in massive stars. In the framework of this programme, we carried out low-resolution spectropolarimetric observations of a large sample of massive stars using FORS2 installed at the ESO VLT 8-m telescope. We determined the magn… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.04502v1-abstract-full').style.display = 'inline'; document.getElementById('1611.04502v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1611.04502v1-abstract-full" style="display: none;"> The "B fields in OB stars" (BOB) collaboration is based on an ESO Large Programme, to study the occurrence rate, properties, and ultimately the origin of magnetic fields in massive stars. In the framework of this programme, we carried out low-resolution spectropolarimetric observations of a large sample of massive stars using FORS2 installed at the ESO VLT 8-m telescope. We determined the magnetic field values with two completely independent reduction and analysis pipelines. Our in-depth study of the magnetic field measurements shows that differences between our two pipelines are usually well within 3sigma errors. From the 32 observations of 28 OB stars, we were able to monitor the magnetic fields in CPD-57 3509 and HD164492C, confirm the magnetic field in HD54879, and detect a magnetic field in CPD-62 2124. We obtain a magnetic field detection rate of 6+-3% for the full sample of 69 OB stars observed with FORS2 within the BOB programme. For the pre-selected objects with a v sin i below 60 km/s, we obtain a magnetic field detection rate of 5+-5%. We also discuss X-ray properties and multiplicity of the objects in our FORS2 sample with respect to the magnetic field detections. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.04502v1-abstract-full').style.display = 'none'; document.getElementById('1611.04502v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 November, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">12 pages, 3 tables, 5 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 599, A66 (2017) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1611.02634">arXiv:1611.02634</a> <span> [<a href="https://arxiv.org/pdf/1611.02634">pdf</a>, <a href="https://arxiv.org/format/1611.02634">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"> Physical characterization of Galactic O-type stars targeted by the IACOB and OWN surveys </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Holgado%2C+G">G. Holgado</a>, <a href="/search/astro-ph?searchtype=author&query=Sim%C3%B3n-D%C3%ADaz%2C+S">S. Sim贸n-D铆az</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</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="1611.02634v1-abstract-short" style="display: inline;"> We present first results from the quantitative spectroscopic analysis of 266 Galactic O-type stars targeted by the IACOB and OWN surveys (implying the largest sample of stars of this type analyzed homogeneously). We also evaluate what is the present situation regarding available information about distances, as provided by the Hipparcos and Gaia missions. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1611.02634v1-abstract-full" style="display: none;"> We present first results from the quantitative spectroscopic analysis of 266 Galactic O-type stars targeted by the IACOB and OWN surveys (implying the largest sample of stars of this type analyzed homogeneously). We also evaluate what is the present situation regarding available information about distances, as provided by the Hipparcos and Gaia missions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.02634v1-abstract-full').style.display = 'none'; document.getElementById('1611.02634v1-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, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">To appear in Highlights on Spanish Astrophysics IX, Proceedings of the XII Scientific Meeting of the Spanish Astronomical Society held on July 18-22, 2016, in Bilbao, Spain</span> </p> </li> </ol> <nav class="pagination is-small is-centered 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