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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/?searchtype=author&amp;query=Frost%2C+A+J">A. J. Frost</a>, <a href="/search/?searchtype=author&amp;query=Sana%2C+H">H. Sana</a>, <a href="/search/?searchtype=author&amp;query=Mahy%2C+L">L. Mahy</a>, <a href="/search/?searchtype=author&amp;query=Wade%2C+G">G. Wade</a>, <a href="/search/?searchtype=author&amp;query=Barron%2C+J">J. Barron</a>, <a href="/search/?searchtype=author&amp;query=Bouquin%2C+J+-+L">J. -B. Le Bouquin</a>, <a href="/search/?searchtype=author&amp;query=M%C3%A9rand%2C+A">A. M茅rand</a>, <a href="/search/?searchtype=author&amp;query=Schneider%2C+F+R+N">F. R. N. Schneider</a>, <a href="/search/?searchtype=author&amp;query=Shenar%2C+T">T. Shenar</a>, <a href="/search/?searchtype=author&amp;query=Barb%C3%A1%2C+R+H">R. H. Barb谩</a>, <a href="/search/?searchtype=author&amp;query=Bowman%2C+D+M">D. M. Bowman</a>, <a href="/search/?searchtype=author&amp;query=Fabry%2C+M">M. Fabry</a>, <a href="/search/?searchtype=author&amp;query=Farhang%2C+A">A. Farhang</a>, <a href="/search/?searchtype=author&amp;query=Marchant%2C+P">P. Marchant</a>, <a href="/search/?searchtype=author&amp;query=Morrell%2C+N+I">N. I. Morrell</a>, <a href="/search/?searchtype=author&amp;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&hellip; <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';">&#9661; 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';">&#9651; 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/2403.00547">arXiv:2403.00547</a> <span>&nbsp;[<a href="https://arxiv.org/pdf/2403.00547">pdf</a>, <a href="https://arxiv.org/format/2403.00547">other</a>]&nbsp;</span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The EDIBLES Survey. VIII. Band profile alignment of diffuse interstellar bands </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&amp;query=Ebenbichler%2C+A">A. Ebenbichler</a>, <a href="/search/?searchtype=author&amp;query=Smoker%2C+J+V">J. V. Smoker</a>, <a href="/search/?searchtype=author&amp;query=Lallement%2C+R">R. Lallement</a>, <a href="/search/?searchtype=author&amp;query=Farhang%2C+A">A. Farhang</a>, <a href="/search/?searchtype=author&amp;query=Cox%2C+N+L+J">N. L. J. Cox</a>, <a href="/search/?searchtype=author&amp;query=Joblin%2C+C">C. Joblin</a>, <a href="/search/?searchtype=author&amp;query=van+Loon%2C+J+T">J. Th. van Loon</a>, <a href="/search/?searchtype=author&amp;query=Linnartz%2C+H">H. Linnartz</a>, <a href="/search/?searchtype=author&amp;query=Przybilla%2C+N">N. Przybilla</a>, <a href="/search/?searchtype=author&amp;query=Ehrenfreund%2C+P">P. Ehrenfreund</a>, <a href="/search/?searchtype=author&amp;query=Cami%2C+J">J. Cami</a>, <a href="/search/?searchtype=author&amp;query=Cordiner%2C+M">M. Cordiner</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="2403.00547v1-abstract-short" style="display: inline;"> Context: There have been many attempts to identify families of diffuse interstellar bands (DIBs) with perfectly correlating band strengths. Although major efforts have been made to classify broadly based DIB families and important insights have been gained, no family has been identified with sufficient accuracy or statistical significance to prove that a series of selected DIBs originates from the&hellip; <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.00547v1-abstract-full').style.display = 'inline'; document.getElementById('2403.00547v1-abstract-short').style.display = 'none';">&#9661; More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.00547v1-abstract-full" style="display: none;"> Context: There have been many attempts to identify families of diffuse interstellar bands (DIBs) with perfectly correlating band strengths. Although major efforts have been made to classify broadly based DIB families and important insights have been gained, no family has been identified with sufficient accuracy or statistical significance to prove that a series of selected DIBs originates from the same carrier. This can be attributed in part to the exclusive use of equivalent widths to establish DIB families. Aims: In a change of strategy, we search for DIBs that are highly correlated in both band strength and profile shape. This approach increases the chance of correlating DIBs being members of one family and originating from the same carrier molecule. We also search for correlations between DIB profile families and atomic interstellar lines, with the goal of further chemically constraining possible DIB carriers. Methods: We adapted the well-known method of time-series alignment to perform a spectral alignment; that is, DIB alignment. In a second step, we analysed the alignment results using a clustering analysis. This method required a statistically significant data set of DIB sight lines. The ESO Diffuse Interstellar Bands Large Exploration Survey (EDIBLES) data were perfectly suited for this application. Results: We report eight DIB families with correlating strengths and profiles, as well as four previously unreported DIBs in the visual range, found using DIB alignment. All profile family members show Pearson correlation coefficients in band strength higher than 0.9. In particular, we report the 6614 - 6521 AA DIB pair, in which both DIBs show the same triple-peak substructure and an unprecedented band strength Pearson correlation coefficient of 0.9935. The presented approach opens up new perspectives that can guide the laboratory search for DIB carriers. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.00547v1-abstract-full').style.display = 'none'; document.getElementById('2403.00547v1-abstract-short').style.display = 'inline';">&#9651; Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">53 pages, 53 figures, Accepted for publication in Astronomy &amp; Astrophysics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.06873">arXiv:2305.06873</a> <span>&nbsp;[<a href="https://arxiv.org/pdf/2305.06873">pdf</a>, <a href="https://arxiv.org/format/2305.06873">other</a>]&nbsp;</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/10.1051/0004-6361/202346314">10.1051/0004-6361/202346314 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Determination of small-scale magnetic fields on Sun-like stars in the near-infrared using CRIRES$^+$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&amp;query=Hahlin%2C+A">A. Hahlin</a>, <a href="/search/?searchtype=author&amp;query=Kochukhov%2C+O">O. Kochukhov</a>, <a href="/search/?searchtype=author&amp;query=Rains%2C+A+D">A. D. Rains</a>, <a href="/search/?searchtype=author&amp;query=Lavail%2C+A">A. Lavail</a>, <a href="/search/?searchtype=author&amp;query=Hatzes%2C+A">A. Hatzes</a>, <a href="/search/?searchtype=author&amp;query=Piskunov%2C+N">N. Piskunov</a>, <a href="/search/?searchtype=author&amp;query=Reiners%2C+A">A. Reiners</a>, <a href="/search/?searchtype=author&amp;query=Seemann%2C+U">U. Seemann</a>, <a href="/search/?searchtype=author&amp;query=Boldt-Christmas%2C+L">L. Boldt-Christmas</a>, <a href="/search/?searchtype=author&amp;query=Guenther%2C+E+W">E. W. Guenther</a>, <a href="/search/?searchtype=author&amp;query=Heiter%2C+U">U. Heiter</a>, <a href="/search/?searchtype=author&amp;query=Nortmann%2C+L">L. Nortmann</a>, <a href="/search/?searchtype=author&amp;query=Yan%2C+F">F. Yan</a>, <a href="/search/?searchtype=author&amp;query=Shulyak%2C+D">D. Shulyak</a>, <a href="/search/?searchtype=author&amp;query=Smoker%2C+J+V">J. V. Smoker</a>, <a href="/search/?searchtype=author&amp;query=Rodler%2C+F">F. Rodler</a>, <a href="/search/?searchtype=author&amp;query=Bristow%2C+P">P. Bristow</a>, <a href="/search/?searchtype=author&amp;query=Dorn%2C+R+J">R. J. Dorn</a>, <a href="/search/?searchtype=author&amp;query=Jung%2C+Y">Y. Jung</a>, <a href="/search/?searchtype=author&amp;query=Marquart%2C+T">T. Marquart</a>, <a href="/search/?searchtype=author&amp;query=Stempels%2C+E">E. Stempels</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2305.06873v1-abstract-short" style="display: inline;"> We aim to characterise the small-scale magnetic fields for a sample of 16 Sun-like stars and investigate the capabilities of the newly upgraded near-infrared (NIR) instrument CRIRES$^+$ at the VLT in the context of small-scale magnetic field studies. Our targets also had their magnetic fields studied in the optical, which allows us to compare magnetic field properties at different spatial scales o&hellip; <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.06873v1-abstract-full').style.display = 'inline'; document.getElementById('2305.06873v1-abstract-short').style.display = 'none';">&#9661; More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.06873v1-abstract-full" style="display: none;"> We aim to characterise the small-scale magnetic fields for a sample of 16 Sun-like stars and investigate the capabilities of the newly upgraded near-infrared (NIR) instrument CRIRES$^+$ at the VLT in the context of small-scale magnetic field studies. Our targets also had their magnetic fields studied in the optical, which allows us to compare magnetic field properties at different spatial scales on the stellar surface and to contrast small-scale magnetic field measurements at different wavelengths. We analyse the Zeeman broadening signature for six magnetically sensitive and insensitive \ion{Fe}{I} lines in the H-band to measure small-scale magnetic fields on the stellar surface. We use polarised radiative transfer modelling and NLTE departure coefficients in combination with MCMC to determine magnetic field characteristics together with non-magnetic stellar parameters. We use two different approaches to describe small-scale magnetic fields. The first is a two-component model with a single magnetic region and a free magnetic field strength. The second model contains multiple magnetic components with fixed magnetic field strengths. We find average magnetic field strengths ranging from $\sim 0.4$ kG down to $&lt;0.1$ kG. The results align closely with other results from high resolution NIR spectrographs such as SPIRou. We find that the small-scale fields correlate with the large-scale fields and that the small-scale fields are at least 10 times stronger than the large-scale fields inferred with Zeeman Doppler imaging. The two- and multi-component models produce systematically different results as the strong fields from the multi-component model increase the obtained mean magnetic field strength. When comparing our results with the optical measurements of small-scale fields we find a systematic offset of 2--3 times stronger fields in the optical. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.06873v1-abstract-full').style.display = 'none'; document.getElementById('2305.06873v1-abstract-short').style.display = 'inline';">&#9651; Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages, 23 figures, accepted by A&amp;A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&amp;A 675, A91 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.08736">arXiv:2302.08736</a> <span>&nbsp;[<a href="https://arxiv.org/pdf/2302.08736">pdf</a>, <a href="https://arxiv.org/format/2302.08736">other</a>]&nbsp;</span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202245371">10.1051/0004-6361/202245371 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CRIRES+ detection of CO emissions lines and temperature inversions on the dayside of WASP-18b and WASP-76b </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&amp;query=Yan%2C+F">F. Yan</a>, <a href="/search/?searchtype=author&amp;query=Nortmann%2C+L">L. Nortmann</a>, <a href="/search/?searchtype=author&amp;query=Reiners%2C+A">A. Reiners</a>, <a href="/search/?searchtype=author&amp;query=Piskunov%2C+N">N. Piskunov</a>, <a href="/search/?searchtype=author&amp;query=Hatzes%2C+A">A. Hatzes</a>, <a href="/search/?searchtype=author&amp;query=Seemann%2C+U">U. Seemann</a>, <a href="/search/?searchtype=author&amp;query=Shulyak%2C+D">D. Shulyak</a>, <a href="/search/?searchtype=author&amp;query=Lavail%2C+A">A. Lavail</a>, <a href="/search/?searchtype=author&amp;query=Rains%2C+A+D">A. D. Rains</a>, <a href="/search/?searchtype=author&amp;query=Cont%2C+D">D. Cont</a>, <a href="/search/?searchtype=author&amp;query=Rengel%2C+M">M. Rengel</a>, <a href="/search/?searchtype=author&amp;query=Lesjak%2C+F">F. Lesjak</a>, <a href="/search/?searchtype=author&amp;query=Nagel%2C+E">E. Nagel</a>, <a href="/search/?searchtype=author&amp;query=Kochukhov%2C+O">O. Kochukhov</a>, <a href="/search/?searchtype=author&amp;query=Czesla%2C+S">S. Czesla</a>, <a href="/search/?searchtype=author&amp;query=Boldt-Christmas%2C+L">L. Boldt-Christmas</a>, <a href="/search/?searchtype=author&amp;query=Heiter%2C+U">U. Heiter</a>, <a href="/search/?searchtype=author&amp;query=Smoker%2C+J+V">J. V. Smoker</a>, <a href="/search/?searchtype=author&amp;query=Rodler%2C+F">F. Rodler</a>, <a href="/search/?searchtype=author&amp;query=Bristow%2C+P">P. Bristow</a>, <a href="/search/?searchtype=author&amp;query=Dorn%2C+R+J">R. J. Dorn</a>, <a href="/search/?searchtype=author&amp;query=Jung%2C+Y">Y. Jung</a>, <a href="/search/?searchtype=author&amp;query=Marquart%2C+T">T. Marquart</a>, <a href="/search/?searchtype=author&amp;query=Stempels%2C+E">E. Stempels</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="2302.08736v1-abstract-short" style="display: inline;"> The dayside atmospheres of ultra-hot Jupiters (UHJs) are predicted to possess temperature inversion layers with extremely high temperatures at high altitudes. We observed the dayside thermal emission spectra of WASP-18b and WASP-76b with the new CRIRES+ high-resolution spectrograph at near-infrared wavelengths. Using the cross-correlation technique, we detected strong CO emission lines in both pla&hellip; <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.08736v1-abstract-full').style.display = 'inline'; document.getElementById('2302.08736v1-abstract-short').style.display = 'none';">&#9661; More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.08736v1-abstract-full" style="display: none;"> The dayside atmospheres of ultra-hot Jupiters (UHJs) are predicted to possess temperature inversion layers with extremely high temperatures at high altitudes. We observed the dayside thermal emission spectra of WASP-18b and WASP-76b with the new CRIRES+ high-resolution spectrograph at near-infrared wavelengths. Using the cross-correlation technique, we detected strong CO emission lines in both planets, which confirms the existence of temperature inversions on their dayside hemispheres. The two planets are the first UHJs orbiting F-type stars with CO emission lines detected; previous detections were mostly for UHJs orbiting A-type stars. Evidence of weak H2O emission signals is also found for both planets. We further applied forward-model retrievals on the detected CO lines and retrieved the temperature-pressure profiles along with the CO volume mixing ratios. The retrieved logarithmic CO mixing ratio of WASP-18b (-2.2) is slightly higher than the value predicted by the self-consistent model assuming solar abundance. For WASP-76b, the retrieved CO mixing ratio (-3.6) is broadly consistent with the value of solar abundance. In addition, we included the equatorial rotation velocity (Veq ) in the retrieval when analyzing the line profile broadening. The obtained Veq is 7.0 km/s for WASP-18b and 5.2 km/s for WASP-76b, which are consistent with the tidally locked rotational velocities. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.08736v1-abstract-full').style.display = 'none'; document.getElementById('2302.08736v1-abstract-short').style.display = 'inline';">&#9651; Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 12 figures; accepted for publication in A&amp;A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&amp;A 672, A107 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.08048">arXiv:2301.08048</a> <span>&nbsp;[<a href="https://arxiv.org/pdf/2301.08048">pdf</a>, <a href="https://arxiv.org/format/2301.08048">other</a>]&nbsp;</span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202245217">10.1051/0004-6361/202245217 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CRIRES$^{+}$ on sky at the ESO Very Large Telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&amp;query=Dorn%2C+R+J">R. J. Dorn</a>, <a href="/search/?searchtype=author&amp;query=Bristow%2C+P">P. Bristow</a>, <a href="/search/?searchtype=author&amp;query=Smoker%2C+J+V">J. V. Smoker</a>, <a href="/search/?searchtype=author&amp;query=Rodler%2C+F">F. Rodler</a>, <a href="/search/?searchtype=author&amp;query=Lavail%2C+A">A. Lavail</a>, <a href="/search/?searchtype=author&amp;query=Accardo%2C+M">M. Accardo</a>, <a href="/search/?searchtype=author&amp;query=Ancker%2C+M+v+d">M. van den Ancker</a>, <a href="/search/?searchtype=author&amp;query=Baade%2C+D">D. Baade</a>, <a href="/search/?searchtype=author&amp;query=Baruffolo%2C+A">A. Baruffolo</a>, <a href="/search/?searchtype=author&amp;query=Courtney-Barrer%2C+B">B. Courtney-Barrer</a>, <a href="/search/?searchtype=author&amp;query=Blanco%2C+L">L. Blanco</a>, <a href="/search/?searchtype=author&amp;query=Brucalassi%2C+A">A. Brucalassi</a>, <a href="/search/?searchtype=author&amp;query=Cumani%2C+C">C. Cumani</a>, <a href="/search/?searchtype=author&amp;query=Follert%2C+R">R. Follert</a>, <a href="/search/?searchtype=author&amp;query=Haimerl%2C+A">A. Haimerl</a>, <a href="/search/?searchtype=author&amp;query=Hatzes%2C+A">A. Hatzes</a>, <a href="/search/?searchtype=author&amp;query=Haug%2C+M">M. Haug</a>, <a href="/search/?searchtype=author&amp;query=Heiter%2C+U">U. Heiter</a>, <a href="/search/?searchtype=author&amp;query=Hinterschuster%2C+R">R. Hinterschuster</a>, <a href="/search/?searchtype=author&amp;query=Hubin%2C+N">N. Hubin</a>, <a href="/search/?searchtype=author&amp;query=Ives%2C+D+J">D. J. Ives</a>, <a href="/search/?searchtype=author&amp;query=Jung%2C+Y">Y. Jung</a>, <a href="/search/?searchtype=author&amp;query=Jones%2C+M">M. Jones</a>, <a href="/search/?searchtype=author&amp;query=Kirchbauer%2C+J">J-P. Kirchbauer</a>, <a href="/search/?searchtype=author&amp;query=Klein%2C+B">B. Klein</a> , et al. (27 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="2301.08048v1-abstract-short" style="display: inline;"> The CRyogenic InfraRed Echelle Spectrograph (CRIRES) Upgrade project CRIRES$^{+}$ extended the capabilities of CRIRES. It transformed this VLT instrument into a cross-dispersed spectrograph to increase the wavelength range that is covered simultaneously by up to a factor of ten. In addition, a new detector focal plane array of three Hawaii 2RG detectors with a 5.3 $渭$m cutoff wavelength replaced t&hellip; <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.08048v1-abstract-full').style.display = 'inline'; document.getElementById('2301.08048v1-abstract-short').style.display = 'none';">&#9661; More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.08048v1-abstract-full" style="display: none;"> The CRyogenic InfraRed Echelle Spectrograph (CRIRES) Upgrade project CRIRES$^{+}$ extended the capabilities of CRIRES. It transformed this VLT instrument into a cross-dispersed spectrograph to increase the wavelength range that is covered simultaneously by up to a factor of ten. In addition, a new detector focal plane array of three Hawaii 2RG detectors with a 5.3 $渭$m cutoff wavelength replaced the existing detectors. Amongst many other improvements, a new spectropolarimetric unit was added and the calibration system has been enhanced. The instrument was installed at the VLT on Unit Telescope 3 at the beginning of 2020 and successfully commissioned and verified for science operations during 2021, partly remotely from Europe due to the COVID-19 pandemic. The instrument was subsequently offered to the community from October 2021 onwards. This article describes the performance and capabilities of the upgraded instrument and presents on sky results. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.08048v1-abstract-full').style.display = 'none'; document.getElementById('2301.08048v1-abstract-short').style.display = 'inline';">&#9651; Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astronomy and Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&amp;A 671, A24 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.03563">arXiv:2212.03563</a> <span>&nbsp;[<a href="https://arxiv.org/pdf/2212.03563">pdf</a>, <a href="https://arxiv.org/format/2212.03563">other</a>]&nbsp;</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/10.1051/0004-6361/202142267">10.1051/0004-6361/202142267 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A high resolution study of near-IR diffuse interstellar bands, search for small scale structure, time variability and stellar features </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&amp;query=Smoker%2C+J+V">J. V. Smoker</a>, <a href="/search/?searchtype=author&amp;query=M%C3%BCller%2C+A">A. M眉ller</a>, <a href="/search/?searchtype=author&amp;query=Ibero%2C+A+M">A. Monreal Ibero</a>, <a href="/search/?searchtype=author&amp;query=Elyajouri%2C+M">M. Elyajouri</a>, <a href="/search/?searchtype=author&amp;query=Evans%2C+C+J">C. J. Evans</a>, <a href="/search/?searchtype=author&amp;query=Najarro%2C+F">F. Najarro</a>, <a href="/search/?searchtype=author&amp;query=Farhang%2C+A">A. Farhang</a>, <a href="/search/?searchtype=author&amp;query=Cox%2C+N+L+J">N. L. J. Cox</a>, <a href="/search/?searchtype=author&amp;query=Minniti%2C+J">J. Minniti</a>, <a href="/search/?searchtype=author&amp;query=Smith%2C+K+T">K. T. Smith</a>, <a href="/search/?searchtype=author&amp;query=Pritchard%2C+J">J. Pritchard</a>, <a href="/search/?searchtype=author&amp;query=Lallement%2C+R">R. Lallement</a>, <a href="/search/?searchtype=author&amp;query=Smette%2C+A">A. Smette</a>, <a href="/search/?searchtype=author&amp;query=Boffin%2C+H+M+J">H. M. J. Boffin</a>, <a href="/search/?searchtype=author&amp;query=Cordiner%2C+M">M. Cordiner</a>, <a href="/search/?searchtype=author&amp;query=Cami%2C+J">J. Cami</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="2212.03563v1-abstract-short" style="display: inline;"> Diffuse interstellar bands comprise hundreds of absorption features in the ISM. Most DIBs are observed in the optical, but some are in the IR. We observed 76 early-type stars at R=50,000 and S/N ratios of several hundreds using CRIRES. We measure DIBs around 1318, 1527, 1561, 1565, 1567, 1574 and/or 1624 nm. We detect a total of 6 DIB features and 17 likely stellar features assisted by a CMFGEN mo&hellip; <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.03563v1-abstract-full').style.display = 'inline'; document.getElementById('2212.03563v1-abstract-short').style.display = 'none';">&#9661; More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.03563v1-abstract-full" style="display: none;"> Diffuse interstellar bands comprise hundreds of absorption features in the ISM. Most DIBs are observed in the optical, but some are in the IR. We observed 76 early-type stars at R=50,000 and S/N ratios of several hundreds using CRIRES. We measure DIBs around 1318, 1527, 1561, 1565, 1567, 1574 and/or 1624 nm. We detect a total of 6 DIB features and 17 likely stellar features assisted by a CMFGEN model. We also measured the DIBs at 1318 and 1527 nm using X-shooter towards ten Ceph. variables with 3.2 &lt; E(B-V) &lt; 6.5 and 4 stars at low values of water vapour. Correlation coeffs. of 0.73-0.96 are found comparing NIRDIB eq. width vs. E(B-V) and with r &gt; 0.8 when comparing the NIR and optical DIBs 5705, 5780, 6203, 6283 and 6269 A. The 5797 A DIB is less well correlated with the NIDIBs. The &#34;C60+&#34; DIB at 9632 A is not well correlated with the 1318 nm DIB. Partial correlation coefficients using E(B-V) as the covariate were also determined. For stars earlier than B2, the 1318 nm DIB is affected by an emission line on its blue wing, likely stellar in nature, although we cannot rule out interstellar/circumstellar origin for example caused by by a DIB in emission. The 1318 nm DIB has a red wing and is reasonably well fitted by two gaussians. Neither the component ratios nor separation are correlated with 5780/5797 or E(B-V). EW(1318 nm) correlates with HI with EW(1318 nm)/E(B-V) decreasing with f(H2). Five pairs of stars within 1 am show similar 1318 nm DIB profiles. Variation in 1318 nm is seen in HD 145501/145502 and HD 168607/168625 pairs. CRIRES data for 17 stars separated by 6-14 months and 2 X-shooter sightlines separated by 9.9 yr were analysed. No time-variability is detected in the 5780, 5797 A, 1318 nm or 1527 nm DIBs. Tentative time variation is observed in the C60+ DIBs at 9577 and 9632 A towards HD 183143 although very close to the noise level with confirmation required. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.03563v1-abstract-full').style.display = 'none'; document.getElementById('2212.03563v1-abstract-short').style.display = 'inline';">&#9651; Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publicaion in the main journal of Astronomy and Astrophysics on 25th November 2022</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&amp;A 672, A181 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1811.11153">arXiv:1811.11153</a> <span>&nbsp;[<a href="https://arxiv.org/pdf/1811.11153">pdf</a>, <a href="https://arxiv.org/format/1811.11153">other</a>]&nbsp;</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/sty3304">10.1093/mnras/sty3304 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A remarkable change of the spectrum of the magnetic Of?p star HD 148937 reveals evidence of an eccentric, high-mass binary </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&amp;query=Wade%2C+G+A">G. A. Wade</a>, <a href="/search/?searchtype=author&amp;query=Smoker%2C+J+V">J. V. Smoker</a>, <a href="/search/?searchtype=author&amp;query=Evans%2C+C+J">C. J. Evans</a>, <a href="/search/?searchtype=author&amp;query=Howarth%2C+I+D">I. D. Howarth</a>, <a href="/search/?searchtype=author&amp;query=Barba%2C+R">R. Barba</a>, <a href="/search/?searchtype=author&amp;query=Cox%2C+N+L+J">N. L. J. Cox</a>, <a href="/search/?searchtype=author&amp;query=Morrell%2C+N">N. Morrell</a>, <a href="/search/?searchtype=author&amp;query=Naz%C3%A9%2C+Y">Y. Naz茅</a>, <a href="/search/?searchtype=author&amp;query=Cami%2C+J">J. Cami</a>, <a href="/search/?searchtype=author&amp;query=Farhang%2C+A">A. Farhang</a>, <a href="/search/?searchtype=author&amp;query=Walborn%2C+N+R">N. R. Walborn</a>, <a href="/search/?searchtype=author&amp;query=Arias%2C+J">J. Arias</a>, <a href="/search/?searchtype=author&amp;query=Gamen%2C+R">R. Gamen</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="1811.11153v1-abstract-short" style="display: inline;"> We report new spectroscopic observations of the magnetic Of?p star HD 148937 obtained since 2015 that differ qualitatively from its extensive historical record of weak, periodic spectral variations. This remarkable behaviour represents clear evidence for an unprecedented change in the character of variability of the star. In this paper we describe the new spectral properties and compare them to th&hellip; <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.11153v1-abstract-full').style.display = 'inline'; document.getElementById('1811.11153v1-abstract-short').style.display = 'none';">&#9661; More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1811.11153v1-abstract-full" style="display: none;"> We report new spectroscopic observations of the magnetic Of?p star HD 148937 obtained since 2015 that differ qualitatively from its extensive historical record of weak, periodic spectral variations. This remarkable behaviour represents clear evidence for an unprecedented change in the character of variability of the star. In this paper we describe the new spectral properties and compare them to the previous line profiles. Based on measurements of the radial velocities of the C iii/N iii} emission lines near 4640 脜 and the C iv absorption lines near 5800 脜, we infer that HD 148937 is likely a high-mass, double-lined spectroscopic binary. Combining the spectroscopic orbit with an archival interferometric measurement of the apparent separation of the equal-brightness components, we tentatively conclude that HD 148937 consists of two O-type stars with masses of approximately 34 and $49~M_\odot$, orbiting in an eccentric ($e=0.75$), long-period ($P_{\rm orb}\sim 26$ y) orbit. We discuss the potential relationship of the binary system to the peculiar properties of HD 148937, and propose future observations to refine the orbital and stellar properties. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.11153v1-abstract-full').style.display = 'none'; document.getElementById('1811.11153v1-abstract-short').style.display = 'inline';">&#9651; Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 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">12 pages, accepted by MNRAS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> MNRAS, 483, 2581-2591 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1811.08662">arXiv:1811.08662</a> <span>&nbsp;[<a href="https://arxiv.org/pdf/1811.08662">pdf</a>, <a href="https://arxiv.org/format/1811.08662">other</a>]&nbsp;</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/10.1051/0004-6361/201833039">10.1051/0004-6361/201833039 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The EDIBLES survey IV. Cosmic ray ionization rates in diffuse clouds from near-ultraviolet observations of interstellar OH$^+$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&amp;query=Bacalla%2C+X+L">Xavier L. Bacalla</a>, <a href="/search/?searchtype=author&amp;query=Linnartz%2C+H">Harold Linnartz</a>, <a href="/search/?searchtype=author&amp;query=Cox%2C+N+L+J">Nick L. J. Cox</a>, <a href="/search/?searchtype=author&amp;query=Cami%2C+J">Jan Cami</a>, <a href="/search/?searchtype=author&amp;query=Roueff%2C+E">Evelyne Roueff</a>, <a href="/search/?searchtype=author&amp;query=Smoker%2C+J+V">Jonathan V. Smoker</a>, <a href="/search/?searchtype=author&amp;query=Farhang%2C+A">Amin Farhang</a>, <a href="/search/?searchtype=author&amp;query=Bouwman%2C+J">Jordy Bouwman</a>, <a href="/search/?searchtype=author&amp;query=Zhao%2C+D">Dongfeng Zhao</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="1811.08662v1-abstract-short" style="display: inline;"> We report cosmic ray ionization rates towards ten reddened stars studied within the framework of the EDIBLES (ESO Diffuse Interstellar Bands Large Exploration Survey) program, using the VLT-UVES. For each sightline, between 2 and 10 individual rotational lines of OH$^+$ have been detected in its (0,0) and (1,0) $A^3螤-X^3危^-$ electronic band system. This allows constraining of OH$^+$ column densiti&hellip; <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.08662v1-abstract-full').style.display = 'inline'; document.getElementById('1811.08662v1-abstract-short').style.display = 'none';">&#9661; More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1811.08662v1-abstract-full" style="display: none;"> We report cosmic ray ionization rates towards ten reddened stars studied within the framework of the EDIBLES (ESO Diffuse Interstellar Bands Large Exploration Survey) program, using the VLT-UVES. For each sightline, between 2 and 10 individual rotational lines of OH$^+$ have been detected in its (0,0) and (1,0) $A^3螤-X^3危^-$ electronic band system. This allows constraining of OH$^+$ column densities towards different objects. Results are also presented for 28 additional sightlines for which only one or rather weak signals are found. An analysis of these data makes it possible to derive the primary cosmic ray ionization rate $味_p$ in the targeted diffuse interstellar clouds. For the ten selected targets, we obtain a range of values for $味_p$ equal to $(3.9-16.4) \times 10^{-16}~\mathrm{s}^{-1}$. These values are higher than the numbers derived in previous detections of interstellar OH$^+$ in the far-infrared / sub-millimeter-wave regions and in other near-ultraviolet studies. This difference is a result of using new OH$^+$ oscillator strength values and a more complete picture of all relevant OH$^+$ formation and destruction routes (including the effect of proton recombinations on PAHs), and the relatively high $N$(OH$^+$) seen toward those ten targets. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.08662v1-abstract-full').style.display = 'none'; document.getElementById('1811.08662v1-abstract-short').style.display = 'inline';">&#9651; Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 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">Journal ref:</span> A&amp;A 622, A31 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1805.11566">arXiv:1805.11566</a> <span>&nbsp;[<a href="https://arxiv.org/pdf/1805.11566">pdf</a>, <a href="https://arxiv.org/format/1805.11566">other</a>]&nbsp;</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/10.1051/0004-6361/201833105">10.1051/0004-6361/201833105 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The EDIBLES survey III. C2-DIBs and their profiles </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&amp;query=Elyajouri%2C+M">M. Elyajouri</a>, <a href="/search/?searchtype=author&amp;query=Lallement%2C+R">R. Lallement</a>, <a href="/search/?searchtype=author&amp;query=Cox%2C+N+L+J">N. L. J. Cox</a>, <a href="/search/?searchtype=author&amp;query=Cami%2C+J">J. Cami</a>, <a href="/search/?searchtype=author&amp;query=Cordiner%2C+M+A">M. A. Cordiner</a>, <a href="/search/?searchtype=author&amp;query=Smoker%2C+J+V">J. V. Smoker</a>, <a href="/search/?searchtype=author&amp;query=Fahrang%2C+A">A. Fahrang</a>, <a href="/search/?searchtype=author&amp;query=Sarre%2C+P+J">P. J. Sarre</a>, <a href="/search/?searchtype=author&amp;query=Linnartz%2C+H">H. Linnartz</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1805.11566v1-abstract-short" style="display: inline;"> The so-called C2-DIBs are a class of very weak bands that fall in the blue part of the optical spectrum and are associated with high column densities of the C2 molecule. DIB profile structures constrain potential molecular carriers, but their measurement requires high S/N and spectra and the use of sightlines without Doppler splitting, as typical for a single-cloud situation. Spectra from the ESO&hellip; <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.11566v1-abstract-full').style.display = 'inline'; document.getElementById('1805.11566v1-abstract-short').style.display = 'none';">&#9661; More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1805.11566v1-abstract-full" style="display: none;"> The so-called C2-DIBs are a class of very weak bands that fall in the blue part of the optical spectrum and are associated with high column densities of the C2 molecule. DIB profile structures constrain potential molecular carriers, but their measurement requires high S/N and spectra and the use of sightlines without Doppler splitting, as typical for a single-cloud situation. Spectra from the ESO Diffuse Interstellar Bands Large Exploration Survey (EDIBLES) conducted at the VLT (ESO/Paranal) were explored to identify single-cloud and high C2 column sightlines, extract the corresponding C2-DIBs and study their strengths and profiles, and to investigate in detail any sub-structures. The target selection was made based on profile-fitting of the Sodium doublets and the detection of C2 lines. The C2 (2-0) Phillips system was fitted using a physical model of the host cloud. C2 column densities, temperatures as well as gas densities were derived for each sightline. 18 known C2-DIBs and 8 strong non-C2 DIBs were extracted towards 8 targets, comprising 7 single-cloud and one multi-cloud line-of-sights. Correlational studies revealed a tight association of the former group with the C2 columns, whereas the non-C2 DIBs are primarily correlated with reddening. We report three new weak diffuse band candidates. We show for the first time that at least 14 C2-DIBs exhibit spectral sub-structures which are consistent with unresolved rotational branches of molecular carriers. The variability of their peak separations among the bands for a given sightline implies that their carriers are different molecules with quite different sizes. We also illustrate how profiles of the same DIB vary among targets and as a function of physical parameters and provide tables defining the sub-structures to be compared with future models and experimental results. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.11566v1-abstract-full').style.display = 'none'; document.getElementById('1805.11566v1-abstract-short').style.display = 'inline';">&#9651; Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 May, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 15 figures, accepted for publication in A&amp;A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&amp;A 616, A143 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1708.03527">arXiv:1708.03527</a> <span>&nbsp;[<a href="https://arxiv.org/pdf/1708.03527">pdf</a>, <a href="https://arxiv.org/ps/1708.03527">ps</a>, <a href="https://arxiv.org/format/1708.03527">other</a>]&nbsp;</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/10.3847/1538-4357/aa745a">10.3847/1538-4357/aa745a <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Origin of B-Type Runaway Stars: Non-LTE Abundances as a Diagnostic </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&amp;query=McEvoy%2C+C+M">Catherine M. McEvoy</a>, <a href="/search/?searchtype=author&amp;query=Dufton%2C+P+L">Philip L. Dufton</a>, <a href="/search/?searchtype=author&amp;query=Smoker%2C+J+V">Jonathan V. Smoker</a>, <a href="/search/?searchtype=author&amp;query=Lambert%2C+D+L">David L. Lambert</a>, <a href="/search/?searchtype=author&amp;query=Keenan%2C+F+P">Francis P. Keenan</a>, <a href="/search/?searchtype=author&amp;query=Schneider%2C+F+R">Fabian R. Schneider</a>, <a href="/search/?searchtype=author&amp;query=de+Witt%2C+W">Willem-Jan de Witt</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="1708.03527v1-abstract-short" style="display: inline;"> There are two accepted mechanisms to explain the origin of runaway OB-type stars: the Binary Supernova Scenario (BSS), and the Cluster Ejection Scenario (CES). In the former, a supernova explosion within a close binary ejects the secondary star, while in the latter close multi-body interactions in a dense cluster cause one or more of the stars to be ejected from the region at high velocity. Both m&hellip; <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1708.03527v1-abstract-full').style.display = 'inline'; document.getElementById('1708.03527v1-abstract-short').style.display = 'none';">&#9661; More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1708.03527v1-abstract-full" style="display: none;"> There are two accepted mechanisms to explain the origin of runaway OB-type stars: the Binary Supernova Scenario (BSS), and the Cluster Ejection Scenario (CES). In the former, a supernova explosion within a close binary ejects the secondary star, while in the latter close multi-body interactions in a dense cluster cause one or more of the stars to be ejected from the region at high velocity. Both mechanisms have the potential to affect the surface composition of the runaway star. TLUSTY non-LTE model atmosphere calculations have been used to determine atmospheric parameters and carbon, nitrogen, magnesium and silicon abundances for a sample of B-type runaways. These same analytical tools were used by Hunter et al. (2009) for their analysis of 50 B-type open cluster Galactic stars (i.e. non-runaways). Effective temperatures were deduced using the silicon-ionization balance technique, surface gravities from Balmer line profiles and microturbulent velocities derived using the Si spectrum. The runaways show no obvious abundance anomalies when compared with stars in the open clusters. The runaways do show a spread in composition which almost certainly reflects the Galactic abundance gradient and a range in the birthplaces of the runaways in the Galactic disk. Since the observed Galactic abundance gradients of C, N, Mg and Si are of a similar magnitude, the abundance ratios (e.g., N/Mg) are, as obtained, essentially uniform across the sample. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1708.03527v1-abstract-full').style.display = 'none'; document.getElementById('1708.03527v1-abstract-short').style.display = 'inline';">&#9651; Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 August, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal, Volume 842, Number 1, 32 (2017) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1511.00843">arXiv:1511.00843</a> <span>&nbsp;[<a href="https://arxiv.org/pdf/1511.00843">pdf</a>, <a href="https://arxiv.org/ps/1511.00843">ps</a>, <a href="https://arxiv.org/format/1511.00843">other</a>]&nbsp;</span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stv1189">10.1093/mnras/stv1189 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Large and small-scale structure of the Intermediate and High Velocity Clouds towards the LMC and SMC </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&amp;query=Smoker%2C+J+V">J. V. Smoker</a>, <a href="/search/?searchtype=author&amp;query=Fox%2C+A+J">A. J. Fox</a>, <a href="/search/?searchtype=author&amp;query=Keenan%2C+F+P">F. P. Keenan</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="1511.00843v1-abstract-short" style="display: inline;"> We employ CaII K and NaI D interstellar absorption-line spectroscopy of early-type stars in the Large and Small Magellanic Clouds to investigate the large- and small-scale structure in foreground Intermediate and High Velocity Clouds (I/HVCs). These data include FLAMES-GIRAFFE CaII K observations of 403 stars in four open clusters, plus FEROS or UVES spectra of 156 stars in the LMC and SMC. The FL&hellip; <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.00843v1-abstract-full').style.display = 'inline'; document.getElementById('1511.00843v1-abstract-short').style.display = 'none';">&#9661; More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1511.00843v1-abstract-full" style="display: none;"> We employ CaII K and NaI D interstellar absorption-line spectroscopy of early-type stars in the Large and Small Magellanic Clouds to investigate the large- and small-scale structure in foreground Intermediate and High Velocity Clouds (I/HVCs). These data include FLAMES-GIRAFFE CaII K observations of 403 stars in four open clusters, plus FEROS or UVES spectra of 156 stars in the LMC and SMC. The FLAMES observations are amongst the most extensive probes to date of CaII structures on 20 arcsec scales From the FLAMES data within a 0.5 degree field-of-view, the CaII K equivalent width in the I/HVC components towards three clusters varies by factors of &gt;10. There are no detections of molecular gas in absorption at intermediate or high velocities, although molecular absorption is present at LMC and Galactic velocities towards some sightlines. The sightlines show variations in EW exceeding a factor 7 in CH+ towards NGC 1761 over scales of less than 10 arcminutes. The FEROS/UVES data show CaII K I/HVC absorption in $\sim$60 per cent of sightlines. No NaI D is found at non-Magellanic HVC velocities aside from a tentative detection towards the star LHA 120-S 93. The range in the CaII/NaI ratio in I/HVCs is from -0.45 to +1.5 dex, similar to previous measurements for I/HVCs. In ten sightlines we find CaII/OI ratios in I/HVC gas ranging from 0.2 to 1.5 dex below the solar value, indicating either dust or ionisation effects. In nine sightlines I/HVC gas is detected in both HI and CaII, and shows similar CaII/HI ratios to typical I/HVCs, and similar velocities, implying that in these sightlines the two elements form part of the same structure. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.00843v1-abstract-full').style.display = 'none'; document.getElementById('1511.00843v1-abstract-short').style.display = 'inline';">&#9651; Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 November, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2015MNRAS.451.4346S </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1511.00470">arXiv:1511.00470</a> <span>&nbsp;[<a href="https://arxiv.org/pdf/1511.00470">pdf</a>, <a href="https://arxiv.org/ps/1511.00470">ps</a>, <a href="https://arxiv.org/format/1511.00470">other</a>]&nbsp;</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/10.1051/0004-6361/201425190">10.1051/0004-6361/201425190 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The large- and small-scale CaII K structure of the Milky Way from observations of Galactic and Magellanic sightlines </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&amp;query=Smoker%2C+J+V">J. V. Smoker</a>, <a href="/search/?searchtype=author&amp;query=Keenan%2C+F+P">F. P. Keenan</a>, <a href="/search/?searchtype=author&amp;query=Fox%2C+A+J">A. J. Fox</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="1511.00470v1-abstract-short" style="display: inline;"> Aims: By utilising spectra of early-type stellar probes of known distances in the same region of the sky, the large and small-scale (pc) structure of the Galactic ISM can be investigated. This paper determines the variation in line strength of CaII at 3933.661 A, as a function of probe separation for a sample of stars, including many sightlines in the Magellanic Clouds. Methods: FLAMES-GIRAFFE dat&hellip; <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.00470v1-abstract-full').style.display = 'inline'; document.getElementById('1511.00470v1-abstract-short').style.display = 'none';">&#9661; More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1511.00470v1-abstract-full" style="display: none;"> Aims: By utilising spectra of early-type stellar probes of known distances in the same region of the sky, the large and small-scale (pc) structure of the Galactic ISM can be investigated. This paper determines the variation in line strength of CaII at 3933.661 A, as a function of probe separation for a sample of stars, including many sightlines in the Magellanic Clouds. Methods: FLAMES-GIRAFFE data taken with the VLT towards early-type stars in 3 Galactic &amp; 4 Magellanic open clusters in CaII are used to obtain the velocity, EW, column density and line width of IS Galactic Ca for a total of 657 stars, of which 443 are Magellanic sightlines. In each cluster there are 43-110 stars observed. Additionally, FEROS and UVES CaII &amp; NaI spectra of 21 Galactic &amp; 154 Magellanic early-type stars are presented and combined with data from the literature to study the Ca column density/parallax relationship. Results: For the four Magellanic clusters studied with FLAMES, the strength of the Galactic IS CaII K EW over transverse scales from 0.05-9 pc is found to vary by factors of 1.8-3.0, corresponding to column density variations of 0.3-0.5 dex in the optically-thin approximation. Using FLAMES, FEROS and UVES archive spectra, the min and max reduced EW for MW gas is found to lie in the range 35-125 mA &amp; 30-160 mA for CaII K and NaI D, respectively. The range is consistent with a simple model of the ISM published by van Loon et al. (2009) consisting of spherical cloudlets of filling factor 0.3, although other geometries are not ruled out. Finally, the derived functional form for parallax and CaII column density is found to be pi(mas)=1/(2.39e-13 x N(CaII)(cm-2)+0.11). Our derived parallax is 25 per cent lower than predicted by Megier et al. (2009) at a distance of 100 pc and 15% lower at a distance of 200 pc, reflecting inhomogeneity in the CaII distribution in the different sightlines studied. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.00470v1-abstract-full').style.display = 'none'; document.getElementById('1511.00470v1-abstract-short').style.display = 'inline';">&#9651; Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 November, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">The full version including online material is available via the Astronomy and Astrophysics website http://www.aanda.org/articles/aa/olm/2015/10/aa25190-14/aa25190-14.html</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2015A&amp;A...582A..59S </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1506.01348">arXiv:1506.01348</a> <span>&nbsp;[<a href="https://arxiv.org/pdf/1506.01348">pdf</a>, <a href="https://arxiv.org/format/1506.01348">other</a>]&nbsp;</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/stv945">10.1093/mnras/stv945 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Early-type stars observed in the ESO UVES Paranal Observatory Project - V. Time-variable interstellar absorption </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&amp;query=McEvoy%2C+C+M">Catherine M. McEvoy</a>, <a href="/search/?searchtype=author&amp;query=Smoker%2C+J+V">Jonathan V. Smoker</a>, <a href="/search/?searchtype=author&amp;query=Dufton%2C+P+L">Philip L. Dufton</a>, <a href="/search/?searchtype=author&amp;query=Smith%2C+K+T">Keith T. Smith</a>, <a href="/search/?searchtype=author&amp;query=Kennedy%2C+M+B">Michael B. Kennedy</a>, <a href="/search/?searchtype=author&amp;query=Keenan%2C+F+P">Francis P. Keenan</a>, <a href="/search/?searchtype=author&amp;query=Lambert%2C+D+L">David L. Lambert</a>, <a href="/search/?searchtype=author&amp;query=Welty%2C+D+E">Daniel E. Welty</a>, <a href="/search/?searchtype=author&amp;query=Lauroesch%2C+J+T">James T. Lauroesch</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="1506.01348v1-abstract-short" style="display: inline;"> The structure and properties of the diffuse interstellar medium (ISM) on small scales, sub-au to 1 pc, are poorly understood. We compare interstellar absorption-lines, observed towards a selection of O- and B-type stars at two or more epochs, to search for variations over time caused by the transverse motion of each star combined with changes in the structure in the foreground ISM. Two sets of dat&hellip; <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1506.01348v1-abstract-full').style.display = 'inline'; document.getElementById('1506.01348v1-abstract-short').style.display = 'none';">&#9661; More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1506.01348v1-abstract-full" style="display: none;"> The structure and properties of the diffuse interstellar medium (ISM) on small scales, sub-au to 1 pc, are poorly understood. We compare interstellar absorption-lines, observed towards a selection of O- and B-type stars at two or more epochs, to search for variations over time caused by the transverse motion of each star combined with changes in the structure in the foreground ISM. Two sets of data were used: 83 VLT- UVES spectra with approximately 6 yr between epochs and 21 McDonald observatory 2.7m telescope echelle spectra with 6 - 20 yr between epochs, over a range of scales from 0 - 360 au. The interstellar absorption-lines observed at the two epochs were subtracted and searched for any residuals due to changes in the foreground ISM. Of the 104 sightlines investigated with typically five or more components in Na I D, possible temporal variation was identified in five UVES spectra (six components), in Ca II, Ca I and/or Na I absorption-lines. The variations detected range from 7\% to a factor of 3.6 in column density. No variation was found in any other interstellar species. Most sightlines show no variation, with 3蟽 upper limits to changes of the order 0.1 - 0.3 dex in Ca II and Na I. These variations observed imply that fine-scale structure is present in the ISM, but at the resolution available in this study, is not very common at visible wavelengths. A determination of the electron densities and lower limits to the total number density of a sample of the sightlines implies that there is no striking difference between these parameters in sightlines with, and sightlines without, varying components. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1506.01348v1-abstract-full').style.display = 'none'; document.getElementById('1506.01348v1-abstract-short').style.display = 'inline';">&#9651; Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 June, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 11 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/1401.2628">arXiv:1401.2628</a> <span>&nbsp;[<a href="https://arxiv.org/pdf/1401.2628">pdf</a>, <a href="https://arxiv.org/ps/1401.2628">ps</a>, <a href="https://arxiv.org/format/1401.2628">other</a>]&nbsp;</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/10.1051/0004-6361/201322421">10.1051/0004-6361/201322421 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The yellow hypergiant HR 5171 A: Resolving a massive interacting binary in the common envelope phase </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&amp;query=Chesneau%2C+O">O. Chesneau</a>, <a href="/search/?searchtype=author&amp;query=Meilland%2C+A">A. Meilland</a>, <a href="/search/?searchtype=author&amp;query=Chapellier%2C+E">E. Chapellier</a>, <a href="/search/?searchtype=author&amp;query=Millour%2C+F">F. Millour</a>, <a href="/search/?searchtype=author&amp;query=Van+Genderen%2C+A+M">A. M. Van Genderen</a>, <a href="/search/?searchtype=author&amp;query=Naz%C3%A9%2C+Y">Y. Naz茅</a>, <a href="/search/?searchtype=author&amp;query=Smith%2C+N">N. Smith</a>, <a href="/search/?searchtype=author&amp;query=Spang%2C+A">A. Spang</a>, <a href="/search/?searchtype=author&amp;query=Smoker%2C+J+V">J. V. Smoker</a>, <a href="/search/?searchtype=author&amp;query=Dessart%2C+L">L. Dessart</a>, <a href="/search/?searchtype=author&amp;query=Kanaan%2C+S">S. Kanaan</a>, <a href="/search/?searchtype=author&amp;query=Bendjoya%2C+P">Ph. Bendjoya</a>, <a href="/search/?searchtype=author&amp;query=Feast%2C+M+W">M. W. Feast</a>, <a href="/search/?searchtype=author&amp;query=Groh%2C+J+H">J. H. Groh</a>, <a href="/search/?searchtype=author&amp;query=Lobel%2C+A">A. Lobel</a>, <a href="/search/?searchtype=author&amp;query=Nardetto%2C+N">N. Nardetto</a>, <a href="/search/?searchtype=author&amp;query=Otero%2C+S">S. Otero</a>, <a href="/search/?searchtype=author&amp;query=Oudmaijer%2C+R+D">R. D. Oudmaijer</a>, <a href="/search/?searchtype=author&amp;query=Tekola%2C+A+G">A. G. Tekola</a>, <a href="/search/?searchtype=author&amp;query=Whitelock%2C+P+A">P. A. Whitelock</a>, <a href="/search/?searchtype=author&amp;query=Arcos%2C+C">C. Arcos</a>, <a href="/search/?searchtype=author&amp;query=Cur%C3%A9%2C+M">M. Cur茅</a>, <a href="/search/?searchtype=author&amp;query=Vanzi%2C+L">L. Vanzi</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="1401.2628v2-abstract-short" style="display: inline;"> We initiated long-term optical interferometry monitoring of the diameters of unstable yellow hypergiants (YHG) with the goal of detecting both the long-term evolution of their radius and shorter term formation related to large mass-loss events. We observed HR5171 A with AMBER/VLTI. We also examined archival photometric data in the visual and near-IR spanning more than 60 years, as well as sparse s&hellip; <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1401.2628v2-abstract-full').style.display = 'inline'; document.getElementById('1401.2628v2-abstract-short').style.display = 'none';">&#9661; More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1401.2628v2-abstract-full" style="display: none;"> We initiated long-term optical interferometry monitoring of the diameters of unstable yellow hypergiants (YHG) with the goal of detecting both the long-term evolution of their radius and shorter term formation related to large mass-loss events. We observed HR5171 A with AMBER/VLTI. We also examined archival photometric data in the visual and near-IR spanning more than 60 years, as well as sparse spectroscopic data. HR5171A exhibits a complex appearance. Our AMBER data reveal a surprisingly large star for a YHG R*=1315+/-260Rsun\ (~6.1AU) at the distance of 3.6+/-0.5kpc. The source is surrounded by an extended nebulosity, and these data also show a large level of asymmetry in the brightness distribution of the system, which we attribute to a newly discovered companion star located in front of the primary star. The companion&#39;s signature is also detected in the visual photometry, which indicates an orbital period of Porb=1304+/-6d. Modeling the light curve with the NIGHTFALL program provides clear evidence that the system is a contact or possibly over-contact eclipsing binary. A total current system mass of 39^{+40}_{-22} solar mass and a high mass ratio q&gt;10 is inferred for the system. The low-mass companion of HR5171 A is very close to the primary star that is embedded within its dense wind. Tight constraints on the inclination and vsini of the primary are lacking, which prevents us from determining its influence precisely on the mass-loss phenomenon, but the system is probably experiencing a wind Roche-Lobe overflow. Depending on the amount of angular momentum that can be transferred to the stellar envelope, HR5171 A may become a fast-rotating B[e]/Luminous Blue Variable (LBV)/Wolf-Rayet star. In any case, HR5171 A highlights the possible importance of binaries for interpreting the unstable YHGs and for massive star evolution in general. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1401.2628v2-abstract-full').style.display = 'none'; document.getElementById('1401.2628v2-abstract-short').style.display = 'inline';">&#9651; Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 January, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 January, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted in Astronomy &amp; Astrophysics (Jan 2014)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&amp;A, 563, A71 (23p, 2014) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1006.0974">arXiv:1006.0974</a> <span>&nbsp;[<a href="https://arxiv.org/pdf/1006.0974">pdf</a>, <a href="https://arxiv.org/ps/1006.0974">ps</a>, <a href="https://arxiv.org/format/1006.0974">other</a>]&nbsp;</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/10.1088/0004-637X/718/2/1046">10.1088/0004-637X/718/2/1046 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Exploring the Origin and Fate of the Magellanic Stream with Ultraviolet and Optical Absorption </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&amp;query=Fox%2C+A+J">Andrew J. Fox</a>, <a href="/search/?searchtype=author&amp;query=Wakker%2C+B+P">Bart P. Wakker</a>, <a href="/search/?searchtype=author&amp;query=Smoker%2C+J+V">Jonathan V. Smoker</a>, <a href="/search/?searchtype=author&amp;query=Richter%2C+P">Philipp Richter</a>, <a href="/search/?searchtype=author&amp;query=Savage%2C+B+D">Blair D. Savage</a>, <a href="/search/?searchtype=author&amp;query=Sembach%2C+K+R">Kenneth R. Sembach</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="1006.0974v1-abstract-short" style="display: inline;"> (Abridged) We present an analysis of ionization and metal enrichment in the Magellanic Stream (MS), the nearest gaseous tidal stream, using HST/STIS and FUSE ultraviolet spectroscopy of two background AGN, NGC 7469 and Mrk 335. For NGC 7469, we include optical spectroscopy from VLT/UVES. In both sightlines the MS is detected in low-ion and high-ion absorption. Toward NGC 7469, we measure a MS oxyg&hellip; <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1006.0974v1-abstract-full').style.display = 'inline'; document.getElementById('1006.0974v1-abstract-short').style.display = 'none';">&#9661; More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1006.0974v1-abstract-full" style="display: none;"> (Abridged) We present an analysis of ionization and metal enrichment in the Magellanic Stream (MS), the nearest gaseous tidal stream, using HST/STIS and FUSE ultraviolet spectroscopy of two background AGN, NGC 7469 and Mrk 335. For NGC 7469, we include optical spectroscopy from VLT/UVES. In both sightlines the MS is detected in low-ion and high-ion absorption. Toward NGC 7469, we measure a MS oxygen abundance [O/H]_MS=[OI/HI]=-1.00+/-0.05(stat)+/-0.08(syst), supporting the view that the Stream originates in the SMC rather than the LMC. We use CLOUDY to model the low-ion phase of the Stream as a photoionized plasma using the observed Si III/Si II and C III/C II ratios. Toward Mrk 335 this yields an ionization parameter log U between -3.45 and -3.15 and a gas density log (n_H/cm^-3) between -2.51 and -2.21. Toward NGC 7469 we derive sub-solar abundance ratios for [Si/O], [Fe/O], and [Al/O], indicating the presence of dust in the MS. The high-ion column densities are too large to be explained by photoionization, but also cannot be explained by a single-temperature collisional-ionization model (equilibrium or non-equilibrium). This suggests the high-ion plasma is multi-phase. Summing over the low-ion and high-ion phases, we derive conservative lower limits on the ratio N(total H II)/N(H I) of &gt;19 toward NGC 7469 and &gt;330 toward Mrk 335, showing that along these two directions the vast majority of the Stream has been ionized. The presence of warm-hot plasma together with the small-scale structure observed at 21 cm provides evidence for an evaporative interaction with the hot Galactic corona. This scenario, predicted by hydrodynamical simulations, suggests that the fate of the MS will be to replenish the Galactic corona with new plasma, rather than to bring neutral fuel to the disk. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1006.0974v1-abstract-full').style.display = 'none'; document.getElementById('1006.0974v1-abstract-short').style.display = 'inline';">&#9651; Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 June, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2010. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJ. 18 pages, 7 figures, all in color</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0801.2534">arXiv:0801.2534</a> <span>&nbsp;[<a href="https://arxiv.org/pdf/0801.2534">pdf</a>, <a href="https://arxiv.org/ps/0801.2534">ps</a>, <a href="https://arxiv.org/format/0801.2534">other</a>]&nbsp;</span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/529574">10.1086/529574 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Metallicity and Physical Conditions in the Magellanic Bridge </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&amp;query=Lehner%2C+N">N. Lehner</a>, <a href="/search/?searchtype=author&amp;query=Howk%2C+J+C">J. C. Howk</a>, <a href="/search/?searchtype=author&amp;query=Keenan%2C+F+P">F. P. Keenan</a>, <a href="/search/?searchtype=author&amp;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="0801.2534v1-abstract-short" style="display: inline;"> We present a new analysis of the diffuse gas in the Magellanic Bridge (RA&gt;3h) based on HST/STIS E140M and FUSE spectra of 2 early-type stars lying within the Bridge and a QSO behind it. We derive the column densities of HI (from Ly伪), NI, OI, ArI, SiII, SII, and FeII of the gas in the Bridge. Using the atomic species, we determine the first gas-phase metallicity of the Magellanic Bridge, [Z/H]=-&hellip; <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0801.2534v1-abstract-full').style.display = 'inline'; document.getElementById('0801.2534v1-abstract-short').style.display = 'none';">&#9661; More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0801.2534v1-abstract-full" style="display: none;"> We present a new analysis of the diffuse gas in the Magellanic Bridge (RA&gt;3h) based on HST/STIS E140M and FUSE spectra of 2 early-type stars lying within the Bridge and a QSO behind it. We derive the column densities of HI (from Ly伪), NI, OI, ArI, SiII, SII, and FeII of the gas in the Bridge. Using the atomic species, we determine the first gas-phase metallicity of the Magellanic Bridge, [Z/H]=-1.02+/-0.07 toward one sightline, and -1.7&lt;[Z/H]&lt;-0.9 toward the other one, a factor 2 or more smaller than the present-day SMC metallicity. Using the metallicity and N(HI), we show that the Bridge gas along our three lines of sight is ~70-90% ionized, despite high HI columns, logN(HI)=19.6-20.1. Possible sources for the ongoing ionization are certainly the hot stars within the Bridge, hot gas (revealed by OVI absorption), and leaking photons from the SMC and LMC. From the analysis of CII*, we deduce that the overall density of the Bridge must be low (&lt;0.03-0.1 cm^-3). We argue that our findings combined with other recent observational results should motivate new models of the evolution of the SMC-LMC-Galaxy system. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0801.2534v1-abstract-full').style.display = 'none'; document.getElementById('0801.2534v1-abstract-short').style.display = 'inline';">&#9651; Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 January, 2008; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2008. </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 the 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/0705.2196">arXiv:0705.2196</a> <span>&nbsp;[<a href="https://arxiv.org/pdf/0705.2196">pdf</a>, <a href="https://arxiv.org/ps/0705.2196">ps</a>, <a href="https://arxiv.org/format/0705.2196">other</a>]&nbsp;</span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1111/j.1365-2966.2007.11916.x">10.1111/j.1365-2966.2007.11916.x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Iron abundances of B-type post-Asymptotic Giant Branch stars in globular clusters: Barnard 29 in M 13 and ROA 5701 in omega Cen </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&amp;query=Thompson%2C+H+M+A">H. M. A. Thompson</a>, <a href="/search/?searchtype=author&amp;query=Keenan%2C+F+P">F. P. Keenan</a>, <a href="/search/?searchtype=author&amp;query=Dufton%2C+P+L">P. L. Dufton</a>, <a href="/search/?searchtype=author&amp;query=Ryans%2C+R+S+I">R. S. I. Ryans</a>, <a href="/search/?searchtype=author&amp;query=Smoker%2C+J+V">J. V. Smoker</a>, <a href="/search/?searchtype=author&amp;query=Lambert%2C+D+L">D. L. Lambert</a>, <a href="/search/?searchtype=author&amp;query=Zijlstra%2C+A+A">A. A. Zijlstra</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="0705.2196v1-abstract-short" style="display: inline;"> High resolution optical and ultraviolet spectra of two B-type post-Asymptotic Giant Branch (post-AGB) stars in globular clusters, Barnard 29 in M 13 and ROA 5701 in omega Cen, have been analysed using model atmosphere techniques. The optical spectra have been obtained with FEROS on the ESO 2.2-m telescope and the 2d-Coud茅 spectrograph on the 2.7-m McDonald telescope, while the ultraviolet observ&hellip; <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0705.2196v1-abstract-full').style.display = 'inline'; document.getElementById('0705.2196v1-abstract-short').style.display = 'none';">&#9661; More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0705.2196v1-abstract-full" style="display: none;"> High resolution optical and ultraviolet spectra of two B-type post-Asymptotic Giant Branch (post-AGB) stars in globular clusters, Barnard 29 in M 13 and ROA 5701 in omega Cen, have been analysed using model atmosphere techniques. The optical spectra have been obtained with FEROS on the ESO 2.2-m telescope and the 2d-Coud茅 spectrograph on the 2.7-m McDonald telescope, while the ultraviolet observations are from the GHRS on the HST. Abundances of light elements (C, N, O, Mg, Al and S) plus Fe have been determined from the optical spectra, while the ultraviolet data provide additional Fe abundance estimates from Fe III absorption lines in the 1875-1900 脜 wavelength region. A general metal underabundance relative to young B-type stars is found for both Barnard 29 and ROA 5701. These results are consistent with the metallicities of the respective clusters, as well as with previous studies of the objects. The derived abundance patterns suggest that the stars have not undergone a gas-dust separation, contrary to previous suggestions, although they may have evolved from the AGB before the onset of the third dredge-up. However, the Fe abundances derived from the HST spectra are lower than those expected from the metallicities of the respective clusters, by 0.5 dex for Barnard 29 and 0.8 dex for ROA 5701. A similar systematic underabundance is also found for other B-type stars in environments of known metallicity, such as the Magellanic Clouds. These results indicate that the Fe III ultraviolet lines may yield abundance values which are systematically too low by typically 0.6 dex and hence such estimates should be treated with caution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0705.2196v1-abstract-full').style.display = 'none'; document.getElementById('0705.2196v1-abstract-short').style.display = 'inline';">&#9651; Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 May, 2007; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2007. </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, 3 figures. Accepted for publication in MNRAS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Mon.Not.Roy.Astron.Soc.378:1619-1632,2007 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0704.1315">arXiv:0704.1315</a> <span>&nbsp;[<a href="https://arxiv.org/pdf/0704.1315">pdf</a>, <a href="https://arxiv.org/ps/0704.1315">ps</a>, <a href="https://arxiv.org/format/0704.1315">other</a>]&nbsp;</span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1111/j.1365-2966.2007.11807.x">10.1111/j.1365-2966.2007.11807.x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observations towards early-type stars in the ESO-POP survey: II -- searches for intermediate and high velocity clouds </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&amp;query=Smoker%2C+J+V">J. V. Smoker</a>, <a href="/search/?searchtype=author&amp;query=Hunter%2C+I">I. Hunter</a>, <a href="/search/?searchtype=author&amp;query=Kalberla%2C+P+M+W">P. M. W. Kalberla</a>, <a href="/search/?searchtype=author&amp;query=Keenan%2C+F+P">F. P. Keenan</a>, <a href="/search/?searchtype=author&amp;query=Morras%2C+R">R. Morras</a>, <a href="/search/?searchtype=author&amp;query=Hanuschik%2C+R">R. Hanuschik</a>, <a href="/search/?searchtype=author&amp;query=Thompson%2C+H+M+A">H. M. A. Thompson</a>, <a href="/search/?searchtype=author&amp;query=Silva%2C+D">D. Silva</a>, <a href="/search/?searchtype=author&amp;query=Bajaja%2C+E">E. Bajaja</a>, <a href="/search/?searchtype=author&amp;query=Poppel%2C+W+G+L">W. G. L. Poppel</a>, <a href="/search/?searchtype=author&amp;query=Arnal%2C+M">M. Arnal</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="0704.1315v1-abstract-short" style="display: inline;"> We present CaII K and TiII optical spectra of early-type stars taken mainly from the UVES Paranal Observatory Project, plus HI 21-cm spectra from the Vila-Elisa and Leiden-Dwingeloo surveys, which are employed to obtain distances to intermediate and high velocity clouds. HI emission at a velocity of -117 km/s towards the sightline HD 30677 with NHI=1.7x10^19 cm-2 has no corresponding CaII K abso&hellip; <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0704.1315v1-abstract-full').style.display = 'inline'; document.getElementById('0704.1315v1-abstract-short').style.display = 'none';">&#9661; More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0704.1315v1-abstract-full" style="display: none;"> We present CaII K and TiII optical spectra of early-type stars taken mainly from the UVES Paranal Observatory Project, plus HI 21-cm spectra from the Vila-Elisa and Leiden-Dwingeloo surveys, which are employed to obtain distances to intermediate and high velocity clouds. HI emission at a velocity of -117 km/s towards the sightline HD 30677 with NHI=1.7x10^19 cm-2 has no corresponding CaII K absorption, which has a signal-to-noise (S/N) ratio of 610. The star has a spectroscopically determined distance of 2.7-kpc, and hence sets this as a firm lower distance limit towards Anti-Centre cloud ACII. Towards another sightline (HD 46185), HI at +122 km/s and NHI=1.2x10^19 cm-2 is seen. The CaII K spectrum has a S/N = 780, although no absorption is observed at the cloud velocity. This similarly places a firm lower distance limit of 2.9-kpc towards this parcel of gas that may be an intermediate velocity cloud. The lack of intermediate velocity (IV) CaII K absorption towards HD 196426 at a S/N = 500 reinforces a lower distance limit of 700-pc towards this part of Complex gp, where NHI is 1.1x10^19 cm-2 and velocity is +78 km/s. Additionally, no IV CaII K is seen in absorption in the spectrum of HD 19445, which is strong in HI with NHI=8x10^19 cm-2 at -42 km/s, placing a firm although uninteresting lower distance limit of 39-pc to this part of IV South. Finally, no HV CaII K absorption is seen towards HD 115363 at a S/N = 410, placing a lower distance of 3.2-kpc towards the HVC gas at velocity of +224 km/s and NHI=5.2x10^19 cm-2. This gas is in the same region of the sky as complex WE (Wakker 2001), but at higher velocities. The non-detection of CaII K absorption sets a lower distance of 3.2-kpc towards the HVC, which is unsurprising if this feature is indeed related to the Magellanic System. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0704.1315v1-abstract-full').style.display = 'none'; document.getElementById('0704.1315v1-abstract-short').style.display = 'inline';">&#9651; Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 April, 2007; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2007. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted by MNRAS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Mon.Not.Roy.Astron.Soc.378:947-954,2007 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0703663">arXiv:astro-ph/0703663</a> <span>&nbsp;[<a href="https://arxiv.org/pdf/astro-ph/0703663">pdf</a>]&nbsp;</span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1038/nature05825">10.1038/nature05825 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A giant outburst two years before the core-collapse of a massive star </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&amp;query=Pastorello%2C+A">A. Pastorello</a>, <a href="/search/?searchtype=author&amp;query=Smartt%2C+S+J">S. J. Smartt</a>, <a href="/search/?searchtype=author&amp;query=Mattila%2C+S">S. Mattila</a>, <a href="/search/?searchtype=author&amp;query=Eldridge%2C+J+J">J. J. Eldridge</a>, <a href="/search/?searchtype=author&amp;query=Young%2C+D">D. Young</a>, <a href="/search/?searchtype=author&amp;query=Itagaki%2C+K">K. Itagaki</a>, <a href="/search/?searchtype=author&amp;query=Yamaoka%2C+H">H. Yamaoka</a>, <a href="/search/?searchtype=author&amp;query=Navasardyan%2C+H">H. Navasardyan</a>, <a href="/search/?searchtype=author&amp;query=Valenti%2C+S">S. Valenti</a>, <a href="/search/?searchtype=author&amp;query=Patat%2C+F">F. Patat</a>, <a href="/search/?searchtype=author&amp;query=Agnoletto%2C+I">I. Agnoletto</a>, <a href="/search/?searchtype=author&amp;query=Augusteijn%2C+T">T. Augusteijn</a>, <a href="/search/?searchtype=author&amp;query=Benetti%2C+S">S. Benetti</a>, <a href="/search/?searchtype=author&amp;query=Cappellaro%2C+E">E. Cappellaro</a>, <a href="/search/?searchtype=author&amp;query=Boles%2C+T">T. Boles</a>, <a href="/search/?searchtype=author&amp;query=Bonnet-Bidaud%2C+J+-">J. -M. Bonnet-Bidaud</a>, <a href="/search/?searchtype=author&amp;query=Botticella%2C+M+T">M. T. Botticella</a>, <a href="/search/?searchtype=author&amp;query=Bufano%2C+F">F. Bufano</a>, <a href="/search/?searchtype=author&amp;query=Cao%2C+C">C. Cao</a>, <a href="/search/?searchtype=author&amp;query=Deng%2C+J">J. Deng</a>, <a href="/search/?searchtype=author&amp;query=Dennefeld%2C+M">M. Dennefeld</a>, <a href="/search/?searchtype=author&amp;query=Elias-Rosa%2C+N">N. Elias-Rosa</a>, <a href="/search/?searchtype=author&amp;query=Harutyunyan%2C+A">A. Harutyunyan</a>, <a href="/search/?searchtype=author&amp;query=Keenan%2C+F+P">F. P. Keenan</a>, <a href="/search/?searchtype=author&amp;query=Iijima%2C+T">T. Iijima</a> , et al. (10 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0703663v2-abstract-short" style="display: inline;"> The death of massive stars produces a variety of supernovae, which are linked to the structure of the exploding stars. The detection of several precursor stars of Type II supernovae have been reported, however we do not yet have direct information on the progenitors of the hydrogen deficient Type Ib and Ic supernovae. Here we report that the peculiar Type Ib supernova SN2006jc is spatially coinc&hellip; <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0703663v2-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0703663v2-abstract-short').style.display = 'none';">&#9661; More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0703663v2-abstract-full" style="display: none;"> The death of massive stars produces a variety of supernovae, which are linked to the structure of the exploding stars. The detection of several precursor stars of Type II supernovae have been reported, however we do not yet have direct information on the progenitors of the hydrogen deficient Type Ib and Ic supernovae. Here we report that the peculiar Type Ib supernova SN2006jc is spatially coincident with a bright optical transient that occurred in 2004. Spectroscopic and photometric monitoring of the supernova leads us to suggest that the progenitor was a carbon-oxygen Wolf-Rayet star embedded within a helium-rich circumstellar medium. There are different possible explanations for this pre-explosion transient. It appears similar to the giant outbursts of Luminous Blue Variables (LBV) of 60-100 solar mass stars, however the progenitor of SN2006jc was helium and hydrogen deficient. An LBV-like outburst of a Wolf-Rayet star could be invoked, but this would be the first observational evidence of such a phenomenon. Alternatively a massive binary system composed of an LBV which erupted in 2004, and a Wolf-Rayet star exploding as SN2006jc, could explain the observations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0703663v2-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0703663v2-abstract-short').style.display = 'inline';">&#9651; Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 March, 2007; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 March, 2007; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2007. </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, 4 figures (supplementary information included). Originally submitted on Nov. 24, 2006; twice revised. Final version submitted to Nature</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nature447:829-832,2007 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0605223">arXiv:astro-ph/0605223</a> <span>&nbsp;[<a href="https://arxiv.org/pdf/astro-ph/0605223">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0605223">ps</a>, <a href="https://arxiv.org/format/astro-ph/0605223">other</a>]&nbsp;</span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1111/J.1365-2966.2006.10257.X">10.1111/J.1365-2966.2006.10257.X <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A non-LTE abundance analysis of the post-AGB star ROA 5701 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&amp;query=Thompson%2C+H+M+A">H. M. A. Thompson</a>, <a href="/search/?searchtype=author&amp;query=Keenan%2C+F+P">F. P. Keenan</a>, <a href="/search/?searchtype=author&amp;query=Dufton%2C+P+L">P. L. Dufton</a>, <a href="/search/?searchtype=author&amp;query=Ryans%2C+R+S+I">R. S. I. Ryans</a>, <a href="/search/?searchtype=author&amp;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="astro-ph/0605223v1-abstract-short" style="display: inline;"> An analysis of high-resolution Anglo-Australian Telescope (AAT)/ University College London Echelle Spectrograph (UCLES) optical spectra for the ultraviolet (UV)-bright star ROA 5701 in the globular cluster omega Cen (NGC 5139) is performed, using non-local thermodynamic equilibrium (non-LTE) model atmospheres to estimate stellar atmospheric parameters and chemical composition. Abundances are der&hellip; <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0605223v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0605223v1-abstract-short').style.display = 'none';">&#9661; More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0605223v1-abstract-full" style="display: none;"> An analysis of high-resolution Anglo-Australian Telescope (AAT)/ University College London Echelle Spectrograph (UCLES) optical spectra for the ultraviolet (UV)-bright star ROA 5701 in the globular cluster omega Cen (NGC 5139) is performed, using non-local thermodynamic equilibrium (non-LTE) model atmospheres to estimate stellar atmospheric parameters and chemical composition. Abundances are derived for C, N, O, Mg, Si and S, and compared with those found previously by Moehler et al. We find a general metal underabundance relative to young B-type stars, consistent with the average metallicity of the cluster. Our results indicate that ROA 5701 has not undergone a gas-dust separation scenario as previously suggested. However, its abundance pattern does imply that ROA 5701 has evolved off the AGB prior to the onset of the third dredge-up. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0605223v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0605223v1-abstract-short').style.display = 'inline';">&#9651; Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 May, 2006; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2006. </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, 2 figures. Accepted for publication in MNRAS (Online Early)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Mon.Not.Roy.Astron.Soc.368:1749-1756,2006 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0604100">arXiv:astro-ph/0604100</a> <span>&nbsp;[<a href="https://arxiv.org/pdf/astro-ph/0604100">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0604100">ps</a>, <a href="https://arxiv.org/format/astro-ph/0604100">other</a>]&nbsp;</span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361:20053905">10.1051/0004-6361:20053905 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Abundance analysis of 5 early-type stars in the young open cluster IC2391 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&amp;query=Stuetz%2C+C">Ch. Stuetz</a>, <a href="/search/?searchtype=author&amp;query=Bagnulo%2C+S">S. Bagnulo</a>, <a href="/search/?searchtype=author&amp;query=Jehin%2C+E">E. Jehin</a>, <a href="/search/?searchtype=author&amp;query=Ledoux%2C+C">C. Ledoux</a>, <a href="/search/?searchtype=author&amp;query=Cabanac%2C+R">R. Cabanac</a>, <a href="/search/?searchtype=author&amp;query=Melo%2C+C">C. Melo</a>, <a href="/search/?searchtype=author&amp;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="astro-ph/0604100v1-abstract-short" style="display: inline;"> It is unclear whether chemically peculiar stars of the upper main sequence represent a class completely distinct from normal A-type stars, or whether there exists a continuous transition from the normal to the most peculiar late F- to early B-type stars. A systematic abundance analysis of open cluster early-type stars would help to relate the observed differences of the chemical abundances of th&hellip; <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0604100v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0604100v1-abstract-short').style.display = 'none';">&#9661; More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0604100v1-abstract-full" style="display: none;"> It is unclear whether chemically peculiar stars of the upper main sequence represent a class completely distinct from normal A-type stars, or whether there exists a continuous transition from the normal to the most peculiar late F- to early B-type stars. A systematic abundance analysis of open cluster early-type stars would help to relate the observed differences of the chemical abundances of the photospheres to other stellar characteristics, without being concerned by possible different original chemical composition. Furthermore, if a continuous transition region from the very peculiar to the so called normal A-F stars exists, it should be possible to detect objects with mild peculiarities. As a first step of a larger project, an abundance analysis of 5 F-A type stars in the young cluster IC2391 was performed using high resolution spectra obtained with the UVES instrument of the ESO VLT. Our targets seem to follow a general abundance pattern: close to solar abundance of the light elements and iron peak elements, heavy elements are slightly overabundant with respect to the sun, similar to what was found in previous studies of normal field A-type stars of the galactic plane. We detected a weakly chemically peculiar star, HD74044. Its element pattern contains characteristics of CP1 as well as CP2 stars, enhanced abundances of iron peak elements and also higher abundances of Sc, Y, Ba and Ce. We did not detect a magnetic field in this star (detection limit was 2kG). We also studied the star SHJM2, proposed as a pre-main sequence object in previous works. Using spectroscopy we found a high surface gravity, which suggests that the star is very close to the ZAMS. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0604100v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0604100v1-abstract-short').style.display = 'inline';">&#9651; Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 April, 2006; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2006. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages + online material</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0601363">arXiv:astro-ph/0601363</a> <span>&nbsp;[<a href="https://arxiv.org/pdf/astro-ph/0601363">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0601363">ps</a>, <a href="https://arxiv.org/format/astro-ph/0601363">other</a>]&nbsp;</span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1111/j.1365-2966.2006.10054.x">10.1111/j.1365-2966.2006.10054.x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Early-type stars observed in the ESO UVES Paranal Observatory Project: I -- Interstellar Na I UV, Ti II and Ca II K observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&amp;query=Hunter%2C+I">I. Hunter</a>, <a href="/search/?searchtype=author&amp;query=Smoker%2C+J+V">J. V. Smoker</a>, <a href="/search/?searchtype=author&amp;query=Keenan%2C+F+P">F. P. Keenan</a>, <a href="/search/?searchtype=author&amp;query=Ledoux%2C+C">C. Ledoux</a>, <a href="/search/?searchtype=author&amp;query=Jehin%2C+E">E. Jehin</a>, <a href="/search/?searchtype=author&amp;query=Cabanac%2C+R">R. Cabanac</a>, <a href="/search/?searchtype=author&amp;query=Melo%2C+C">C. Melo</a>, <a href="/search/?searchtype=author&amp;query=Bagnulo%2C+S">S. Bagnulo</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="astro-ph/0601363v1-abstract-short" style="display: inline;"> We present an analysis of interstellar Na I (lambda=3302.37脜, 3302.98脜), Ti II (lambda=3383.76脜) and Ca II K (lambda=3933.66脜) absorption features for 74 sightlines towards O- and B-type stars in the Galactic disc. The data were obtained from the UVES Paranal Observatory Project, at a spectral resolution of 3.75km/s and with mean signal to noise ratios per pixel of 260, 300 and 430 for the Na I,&hellip; <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0601363v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0601363v1-abstract-short').style.display = 'none';">&#9661; More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0601363v1-abstract-full" style="display: none;"> We present an analysis of interstellar Na I (lambda=3302.37脜, 3302.98脜), Ti II (lambda=3383.76脜) and Ca II K (lambda=3933.66脜) absorption features for 74 sightlines towards O- and B-type stars in the Galactic disc. The data were obtained from the UVES Paranal Observatory Project, at a spectral resolution of 3.75km/s and with mean signal to noise ratios per pixel of 260, 300 and 430 for the Na I, Ti II and Ca II observations, respectively. Interstellar features were detected in all but one of the Ti II sightlines and all of the Ca II sightlines. The dependence of the column density of these three species with distance, height relative to the Galactic plane, H I column density, reddening and depletion relative to the solar abundance has been investigated. We also examine the accuracy of using the Na I column density as an indicator of that for H I. In general we find similar strong correlations for both Ti and Ca, and weaker correlations for Na. Our results confirm the general belief that Ti and Ca occur in the same regions of the interstellar medium and also that the Ti II/Ca II ratio is constant over all parameters. We hence conclude that the absorption properties of Ti and Ca are essentially constant under the general interstellar medium conditions of the Galactic disc. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0601363v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0601363v1-abstract-short').style.display = 'inline';">&#9651; Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 January, 2006; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2006. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted by MNRAS, 36 pages, 14 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Mon.Not.Roy.Astron.Soc. 367 (2006) 1478-1514 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0510507">arXiv:astro-ph/0510507</a> <span>&nbsp;[<a href="https://arxiv.org/pdf/astro-ph/0510507">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0510507">ps</a>, <a href="https://arxiv.org/format/astro-ph/0510507">other</a>]&nbsp;</span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361:20053436">10.1051/0004-6361:20053436 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CaII K observations of QSOs in the line-of-sight to the Magellanic Bridge </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&amp;query=Smoker%2C+J+V">J. V. Smoker</a>, <a href="/search/?searchtype=author&amp;query=Keenan%2C+F+P">F. P. Keenan</a>, <a href="/search/?searchtype=author&amp;query=Thompson%2C+H+M+A">H. M. A. Thompson</a>, <a href="/search/?searchtype=author&amp;query=Bruns%2C+C">C. Bruns</a>, <a href="/search/?searchtype=author&amp;query=Muller%2C+E">E. Muller</a>, <a href="/search/?searchtype=author&amp;query=Lehner%2C+N">N. Lehner</a>, <a href="/search/?searchtype=author&amp;query=Lee%2C+J+-">J. -K. Lee</a>, <a href="/search/?searchtype=author&amp;query=Hunter%2C+I">I. Hunter</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="astro-ph/0510507v1-abstract-short" style="display: inline;"> We describe medium-resolution spectroscopic observations taken with the ESO Multi-Mode Instrument in the CaII K line (3933.661 Angstroms) towards 7 QSOs located in the line-of-sight to the Magellanic Bridge. At a spectral resolution R = 6,000, five of the sightlines have a signal-to-noise ratio of 20 or higher. Definite Ca absorption due to Bridge material is detected towards 3 objects, with pro&hellip; <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0510507v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0510507v1-abstract-short').style.display = 'none';">&#9661; More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0510507v1-abstract-full" style="display: none;"> We describe medium-resolution spectroscopic observations taken with the ESO Multi-Mode Instrument in the CaII K line (3933.661 Angstroms) towards 7 QSOs located in the line-of-sight to the Magellanic Bridge. At a spectral resolution R = 6,000, five of the sightlines have a signal-to-noise ratio of 20 or higher. Definite Ca absorption due to Bridge material is detected towards 3 objects, with probable detection towards two other sightlines. Gas-phase CaII K Bridge and Milky Way abundances or lower limits for the all sightlines are estimated by the use of Parkes 21-cm HI emission line data. These data only have a spatial resolution of 14 arcminutes compared with the optical observations which have milli-arcsecond resolution. With this caveat, for the three objects with sound CaII K detections, we find that the ionic abundance of CaII K relative to HI, A=log(N(CaK)/N(HI)) for low-velocity Galactic gas ranges from -8.3 to -8.8 dex, with HI column densities varying from 3-6x10^20 cm^-2. For Magellanic Bridge gas, the values of A are 0.5 dex higher, ranging from -7.8 to -8.2 dex, with N(HI)=1-5x10^20 cm^-2. Higher values of A correspond to lower values of N(HI), although numbers are small. For the sightline towards B0251--675, the Bridge gas has two different velocities, and in only one of these is CaII K tentatively detected, perhaps indicating gas of a different origin or present-day characteristics (such as dust content), although this conclusion is uncertain and there is the possibility that one of the components could be related to the Magellanic Stream. Higher signal-to-noise CaII K data and higher resolution HI data are required to determine whether A changes with N(HI) over the Bridge and if the implied difference in the metalicity of the two Bridge components towards B0251-675 is real. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0510507v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0510507v1-abstract-short').style.display = 'inline';">&#9651; Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 October, 2005; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2005. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Astronomy and Astrophysics, in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0406038">arXiv:astro-ph/0406038</a> <span>&nbsp;[<a href="https://arxiv.org/pdf/astro-ph/0406038">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0406038">ps</a>, <a href="https://arxiv.org/format/astro-ph/0406038">other</a>]&nbsp;</span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1111/j.1365-2966.2004.08016.x">10.1111/j.1365-2966.2004.08016.x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CaII K interstellar observations towards early disc and halostars - Paper II; distances to IVCs and HVCs </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&amp;query=Smoker%2C+J+V">J. V. Smoker</a>, <a href="/search/?searchtype=author&amp;query=Lynn%2C+B+B">B. B. Lynn</a>, <a href="/search/?searchtype=author&amp;query=Rolleston%2C+W+R+J">W. R. J. Rolleston</a>, <a href="/search/?searchtype=author&amp;query=Kay%2C+H+R+M">H. R. M. Kay</a>, <a href="/search/?searchtype=author&amp;query=Bajaja%2C+E">E. Bajaja</a>, <a href="/search/?searchtype=author&amp;query=Poppel%2C+W+G+L">W. G. L. Poppel</a>, <a href="/search/?searchtype=author&amp;query=Keenan%2C+F+P">F. P. Keenan</a>, <a href="/search/?searchtype=author&amp;query=Kalberla%2C+P+M+W">P. M. W. Kalberla</a>, <a href="/search/?searchtype=author&amp;query=Mooney%2C+C+J">C. J. Mooney</a>, <a href="/search/?searchtype=author&amp;query=Dufton%2C+P+L">P. L. Dufton</a>, <a href="/search/?searchtype=author&amp;query=Ryans%2C+R+S+I">R. S. I. Ryans</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="astro-ph/0406038v1-abstract-short" style="display: inline;"> We compare existing high spectral resolution (R=40,000) CaII K observations towards 88 mainly B-type stars, and new observations at R=10,000 towards 3 stars, with 21-cm HI emission-line profiles, in order to search for optical absorption towards known intermediate and high velocity cloud complexes. Given certain assumptions, limits to the gas phase abundance of CaII are estimated for the cloud c&hellip; <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0406038v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0406038v1-abstract-short').style.display = 'none';">&#9661; More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0406038v1-abstract-full" style="display: none;"> We compare existing high spectral resolution (R=40,000) CaII K observations towards 88 mainly B-type stars, and new observations at R=10,000 towards 3 stars, with 21-cm HI emission-line profiles, in order to search for optical absorption towards known intermediate and high velocity cloud complexes. Given certain assumptions, limits to the gas phase abundance of CaII are estimated for the cloud components. We use the data to derive the following distances from the Galactic plane (z); 1) Tentative lower z-height limits of 2800 pc and 4100 pc towards Complex C using lack of absorption in the spectra of HD 341617 and PG 0855+294. 2) A weak lower z-height of 1400 pc towards Complex WA-WB using lack of absorption in EC 09470-1433 and weak lower limit of 2470 pc with EC 09452-1403. 3) An upper z-height of 2470 pc towards a southern intermediate velocity cloud (IVC) with v_LSR=-55 km/s using PG 2351+198. 4) Detection of a possible IVC in CaK absorption at v_LSR=+52 km/s using EC 20104-2944. No associated HI in emission is detected. At this position, normal Galactic rotation predicts velocities of up to +25 km/s. The detection puts an upper z-height of 1860 pc to the cloud. 5) Tentative HI and CaK detections towards an IVC at +70 km/s in the direction of HVC Complex WE, sightline EC 06387-8045, indicating that the IVC may be at a z-height lower than 1770 pc. 6) Detection of CaK absorption in the spectrum of PG 0855+294 in the direction of IV20, indicating that this IVC has a z-height smaller than 4100 pc. 7) A weak lower z-height of 4300 pc towards a small HVC with v_LSR=+115 km/s at l,b=200,+52, using lack of absorption in the CaK spectrum of PG 0955+291. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0406038v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0406038v1-abstract-short').style.display = 'inline';">&#9651; Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 June, 2004; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2004. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 5 figures. Accepted for publication in MNRAS, May 13 2004</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Mon.Not.Roy.Astron.Soc. 352 (2004) 1279 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0206373">arXiv:astro-ph/0206373</a> <span>&nbsp;[<a href="https://arxiv.org/pdf/astro-ph/0206373">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0206373">ps</a>, <a href="https://arxiv.org/format/astro-ph/0206373">other</a>]&nbsp;</span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1046/j.1365-8711.2002.05762.x">10.1046/j.1365-8711.2002.05762.x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multiwavelength observations of the M15 intermediate velocity cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&amp;query=Smoker%2C+J+V">J. V. Smoker</a>, <a href="/search/?searchtype=author&amp;query=Haffner%2C+L+M">L. M. Haffner</a>, <a href="/search/?searchtype=author&amp;query=Keenan%2C+F+P">F. P. Keenan</a>, <a href="/search/?searchtype=author&amp;query=Davies%2C+R+D">R. D. Davies</a>, <a href="/search/?searchtype=author&amp;query=Pollacco%2C+D">D. Pollacco</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="astro-ph/0206373v1-abstract-short" style="display: inline;"> We present Westerbork Synthesis Radio Telescope HI images, Lovell Telescope multibeam HI wide-field mapping, Wisconsin H-alpha Mapper facility images, William Herschel Telescope longslit echelle CaII observations, and IRAS ISSA 60 and 100 micron coadded images towards the intermediate velocity cloud located in the general direction of the M15 globular cluster. When combined with previously-publi&hellip; <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0206373v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0206373v1-abstract-short').style.display = 'none';">&#9661; More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0206373v1-abstract-full" style="display: none;"> We present Westerbork Synthesis Radio Telescope HI images, Lovell Telescope multibeam HI wide-field mapping, Wisconsin H-alpha Mapper facility images, William Herschel Telescope longslit echelle CaII observations, and IRAS ISSA 60 and 100 micron coadded images towards the intermediate velocity cloud located in the general direction of the M15 globular cluster. When combined with previously-published Arecibo data, the HI gas in the IVC is found to be clumpy, with peak HI column density of 1.5x10^(20) cm^(-2), inferred volume density (assuming spherical symmetry) of 24 cm^(-3)/(D kpc), and maximum brightness temperature at a resolution of 81x14 arcsec of 14 K. The HI gas in the cloud is warm, with a minimum FWHM value of 5 km/s, corresponding to a kinetic temperature, in the absence of turbulence, of 540 K. There are indications in the HI data of 2-component velocity structure in the IVC, indicative of cloudlets. This velocity structure is also tentatively seen in the CaK spectra, although the SNR is low. The main IVC condensation is detected by WHAM in H-alpha with intensities uncorrected for Galactic absorption of upto 1.3 Rayleigh, indicating that the cloud is partially ionised. The FWHM of the ionised component, at a resolution of 1 degree, exceeds 30 km/s. The spatial and velocity coincidence of the H-alpha and HI peaks in emission is qualitatively good. Finally, the 100 and 60 micron IRAS images show spatial coincidence over a 0.7 degree field, with low and intermediate-velocity gas, respectively, indicating that the IVC may contain dust. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0206373v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0206373v1-abstract-short').style.display = 'inline';">&#9651; Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 June, 2002; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2002. </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">MNRAS, in press</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Mon.Not.Roy.Astron.Soc. 337 (2002) 385 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0204464">arXiv:astro-ph/0204464</a> <span>&nbsp;[<a href="https://arxiv.org/pdf/astro-ph/0204464">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0204464">ps</a>, <a href="https://arxiv.org/format/astro-ph/0204464">other</a>]&nbsp;</span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1046/j.1365-8711.2001.03999.x">10.1046/j.1365-8711.2001.03999.x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Optical spectroscopy of the M15 intermediate velocity cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&amp;query=Smoker%2C+J+V">J. V. Smoker</a>, <a href="/search/?searchtype=author&amp;query=Keenan%2C+F+P">F. P. Keenan</a>, <a href="/search/?searchtype=author&amp;query=Lehner%2C+N">N. Lehner</a>, <a href="/search/?searchtype=author&amp;query=Trundle%2C+C">C. Trundle</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="astro-ph/0204464v1-abstract-short" style="display: inline;"> We present echelle spectrograph observations in NaD, at resolutions of 6.2-8.5 km/s, for 11 stars located in the line-of-sight to the M15 intermediate velocity cloud, which has a radial velocity of 70 km/s. This cloud is a part of IVC Complex gp. The targets range in magnitude from V=13.3-14.8. Seven of the observed stars are in the M15 globular cluster, the remaining four being field stars. Col&hellip; <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0204464v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0204464v1-abstract-short').style.display = 'none';">&#9661; More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0204464v1-abstract-full" style="display: none;"> We present echelle spectrograph observations in NaD, at resolutions of 6.2-8.5 km/s, for 11 stars located in the line-of-sight to the M15 intermediate velocity cloud, which has a radial velocity of 70 km/s. This cloud is a part of IVC Complex gp. The targets range in magnitude from V=13.3-14.8. Seven of the observed stars are in the M15 globular cluster, the remaining four being field stars. Column density ratios of log(N cm^-2)=11.8-12.5 are derived. Combining the current sightlines with previously-existing data, we find the NaD/HI ratio in the IVC varies by upto a factor of 25. One cluster star, M15 ZNG-1, was also observed in Calcium. We find N(CaI)/N(CaII)&lt;0.03 and NaI/CaII=0.25, similar to values seen in the local ISM. Finally, we detect tentative evidence for IV absorption in KI towards 3 cluster stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0204464v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0204464v1-abstract-short').style.display = 'inline';">&#9651; Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 April, 2002; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2002. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">A&amp;A, in press</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Mon.Not.Roy.Astron.Soc. 322 (2001) 13 </p> </li> </ol> <div class="is-hidden-tablet"> <!-- feedback for mobile only --> <span class="help" 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