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</div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.09783">arXiv:2412.09783</a> <span> [<a href="https://arxiv.org/pdf/2412.09783">pdf</a>, <a href="https://arxiv.org/format/2412.09783">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> oMEGACat V: Helium Enrichment in $蠅$ Centauri as a Function of Metallicity </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Clontz%2C+C">C. Clontz</a>, <a href="/search/astro-ph?searchtype=author&query=Seth%2C+A+C">A. C. Seth</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Z">Z. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Souza%2C+S+O">S. O. Souza</a>, <a href="/search/astro-ph?searchtype=author&query=H%C3%A4berle%2C+M">M. H盲berle</a>, <a href="/search/astro-ph?searchtype=author&query=Nitschai%2C+M+S">M. S. Nitschai</a>, <a href="/search/astro-ph?searchtype=author&query=Neumayer%2C+N">N. Neumayer</a>, <a href="/search/astro-ph?searchtype=author&query=Latour%2C+M">M. Latour</a>, <a href="/search/astro-ph?searchtype=author&query=Milone%2C+A+P">A. P. Milone</a>, <a href="/search/astro-ph?searchtype=author&query=Feldmeier-Krause%2C+A">A. Feldmeier-Krause</a>, <a href="/search/astro-ph?searchtype=author&query=Kacharov%2C+N">N. Kacharov</a>, <a href="/search/astro-ph?searchtype=author&query=Libralato%2C+M">M. Libralato</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">A. Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=van+de+Ven%2C+G">G. van de Ven</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro-Cuello%2C+M">M. Alfaro-Cuello</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2412.09783v1-abstract-short" style="display: inline;"> Constraining the helium enhancement in stars is critical for understanding the formation mechanisms of multiple populations in star clusters. However, measuring helium variations for many stars within a cluster remains observationally challenging. We use Hubble Space Telescope photometry combined with MUSE spectroscopic data for over 7,200 red-giant branch stars in \omc\ to measure helium differen… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.09783v1-abstract-full').style.display = 'inline'; document.getElementById('2412.09783v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.09783v1-abstract-full" style="display: none;"> Constraining the helium enhancement in stars is critical for understanding the formation mechanisms of multiple populations in star clusters. However, measuring helium variations for many stars within a cluster remains observationally challenging. We use Hubble Space Telescope photometry combined with MUSE spectroscopic data for over 7,200 red-giant branch stars in \omc\ to measure helium differences between distinct groups of stars as a function of metallicity separating the impact of helium enhancements from other abundance variations on the pseudo-color (chromosome) diagrams. Our results show that stars at all metallicities have subpopulations with significant helium enhancement ($螖Y_{min} \gtrsim$ 0.11). We find a rapid increase in helium enhancement from low metallicities ($\rm{[Fe/H] \simeq -2.05}$ to $\rm{[Fe/H] \simeq -1.92})$, with this enhancement leveling out at \deltay\ $= 0.154$ at higher metallicities. The fraction of helium-enhanced stars steadily increases with metallicity ranging from 10\% at $\rm{[Fe/H] \simeq -2.04}$ to over $90\%$ at $\rm{[Fe/H] \simeq -1.04}$. This study is the first to examine helium enhancement across the full range of metallicities in \omc{}, providing new insight into its formation history and additional constraints on enrichment mechanisms. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.09783v1-abstract-full').style.display = 'none'; document.getElementById('2412.09783v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.13855">arXiv:2409.13855</a> <span> [<a href="https://arxiv.org/pdf/2409.13855">pdf</a>, <a href="https://arxiv.org/format/2409.13855">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> oMEGACat IV: Constraining Ages of Omega Centauri sub-giant branch stars with HST and MUSE </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Clontz%2C+C">C. Clontz</a>, <a href="/search/astro-ph?searchtype=author&query=Seth%2C+A+C">A. C. Seth</a>, <a href="/search/astro-ph?searchtype=author&query=Dotter%2C+A">A. Dotter</a>, <a href="/search/astro-ph?searchtype=author&query=H%C3%A4berle%2C+M">M. H盲berle</a>, <a href="/search/astro-ph?searchtype=author&query=Nitschai%2C+M+S">M. S. Nitschai</a>, <a href="/search/astro-ph?searchtype=author&query=Neumayer%2C+N">N. Neumayer</a>, <a href="/search/astro-ph?searchtype=author&query=Feldmeier-Krause%2C+A">A. Feldmeier-Krause</a>, <a href="/search/astro-ph?searchtype=author&query=Latour%2C+M">M. Latour</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Z">Z. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Souza%2C+S+O">S. O. Souza</a>, <a href="/search/astro-ph?searchtype=author&query=Kacharov%2C+N">N. Kacharov</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">A. Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Libralato%2C+M">M. Libralato</a>, <a href="/search/astro-ph?searchtype=author&query=Pechetti%2C+R">R. Pechetti</a>, <a href="/search/astro-ph?searchtype=author&query=van+de+Ven%2C+G">G. van de Ven</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro-Cuello%2C+M">M. Alfaro-Cuello</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2409.13855v2-abstract-short" style="display: inline;"> We present age estimates for over 8100 sub-giant branch (SGB) stars in Omega Centauri ($蠅$ Cen) to study its star formation history. Our large data set, which combines multi-wavelength HST photometry with MUSE metallicities, provides an unprecedented opportunity to measure individual stellar ages. We do this by fitting each star's photometry and metallicity with theoretical isochrones, that are em… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.13855v2-abstract-full').style.display = 'inline'; document.getElementById('2409.13855v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.13855v2-abstract-full" style="display: none;"> We present age estimates for over 8100 sub-giant branch (SGB) stars in Omega Centauri ($蠅$ Cen) to study its star formation history. Our large data set, which combines multi-wavelength HST photometry with MUSE metallicities, provides an unprecedented opportunity to measure individual stellar ages. We do this by fitting each star's photometry and metallicity with theoretical isochrones, that are embedded with an empirical [C+N+O]-[Fe/H] relation specifically for $蠅$ Cen. The bulk of the stars have ages between 13 and 10 Gyr, with the mean stellar age being 12.08$\pm$0.01 Gyrs and the median age uncertainty being 0.68 Gyrs. From these ages we construct the most complete age-metallicity relation (AMR) for $蠅$ Cen to date. We find that the mean age of stars decreases with increasing metallicity and find two distinct streams in the age-metallicity plane, hinting at different star formation pathways. We derive an intrinsic spread in the ages of 0.75$\pm$0.01 Gyr for the whole cluster, with the age spread showing a clear increase with metallicity. We verify the robustness of our age estimations by varying isochrone parameters and constraining our systematics. We find the C+N+O relation to be the most critical consideration for constraining the AMR. We also present the SGB chromosome map with age information. In the future, these stellar ages could be combined with chemical abundances to study age differences in subpopulations, and uncover the chemical evolution history of this massive nuclear star cluster. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.13855v2-abstract-full').style.display = 'none'; document.getElementById('2409.13855v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 pages, 11 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.17347">arXiv:2406.17347</a> <span> [<a href="https://arxiv.org/pdf/2406.17347">pdf</a>, <a href="https://arxiv.org/format/2406.17347">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Hubble Space Telescope proper motions of Large Magellanic Cloud star clusters -- I. Catalogues and results for NGC 1850 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Niederhofer%2C+F">F. Niederhofer</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">A. Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Kozhurina-Platais%2C+V">V. Kozhurina-Platais</a>, <a href="/search/astro-ph?searchtype=author&query=Libralato%2C+M">M. Libralato</a>, <a href="/search/astro-ph?searchtype=author&query=H%C3%A4berle%2C+M">M. H盲berle</a>, <a href="/search/astro-ph?searchtype=author&query=Kacharov%2C+N">N. Kacharov</a>, <a href="/search/astro-ph?searchtype=author&query=Kamann%2C+S">S. Kamann</a>, <a href="/search/astro-ph?searchtype=author&query=Bastian%2C+N">N. Bastian</a>, <a href="/search/astro-ph?searchtype=author&query=Cabrera-Ziri%2C+I">I. Cabrera-Ziri</a>, <a href="/search/astro-ph?searchtype=author&query=Cioni%2C+M+-+L">M. -R. L. Cioni</a>, <a href="/search/astro-ph?searchtype=author&query=Dresbach%2C+F">F. Dresbach</a>, <a href="/search/astro-ph?searchtype=author&query=Martocchia%2C+S">S. Martocchia</a>, <a href="/search/astro-ph?searchtype=author&query=Massari%2C+D">D. Massari</a>, <a href="/search/astro-ph?searchtype=author&query=Saracino%2C+S">S. Saracino</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.17347v1-abstract-short" style="display: inline;"> We present proper motion (PM) measurements for a sample of 23 massive star clusters within the Large Magellanic Cloud using multi-epoch data from the Hubble Space Telescope (HST). We combined archival data from the ACS/WFC and WFC3/UVIS instruments with observations from a dedicated HST programme, resulting in time baselines between 4.7 and 18.2 yr available for PM determinations. For bright well-… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.17347v1-abstract-full').style.display = 'inline'; document.getElementById('2406.17347v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.17347v1-abstract-full" style="display: none;"> We present proper motion (PM) measurements for a sample of 23 massive star clusters within the Large Magellanic Cloud using multi-epoch data from the Hubble Space Telescope (HST). We combined archival data from the ACS/WFC and WFC3/UVIS instruments with observations from a dedicated HST programme, resulting in time baselines between 4.7 and 18.2 yr available for PM determinations. For bright well-measured stars, we achieved nominal PM precisions of 55 $渭$as/yr down to 11 $渭$as/yr . To demonstrate the potential and limitations of our PM data set, we analysed the cluster NGC 1850 and showcase a selection of different science applications. The precision of the PM measurements allows us to disentangle the kinematics of the various stellar populations that are present in the HST field. The cluster has a centre-of-mass motion that is different from the surrounding old field stars and also differs from the mean motion of a close-by group of very young stars. We determined the velocity dispersion of field stars to be 0.128 +/- 0.003 mas/yr (corresponding to 30.3 +/- 0.7 km/s). The velocity dispersion of the cluster inferred from the PM data set most probably overestimates the true value, suggesting that the precision of the measurements at this stage is not sufficient for a reliable analysis of the internal kinematics of extra-galactic star clusters. Finally, we exploit the PM-cleaned catalogue of likely cluster members to determine any radial segregation between fast and slowly-rotating stars, finding that the former are more centrally concentrated. With this paper, we also release the astro-photometric catalogues for each cluster. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.17347v1-abstract-full').style.display = 'none'; document.getElementById('2406.17347v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">27 pages, 15 figures. Accepted for publication in A&A. Astro-photometric catalogues are available at https://archive.stsci.edu/hlsp/hamsters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.01688">arXiv:2406.01688</a> <span> [<a href="https://arxiv.org/pdf/2406.01688">pdf</a>, <a href="https://arxiv.org/format/2406.01688">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ad5289">10.3847/1538-4357/ad5289 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> oMEGACat III. Multi-band photometry and metallicities reveal spatially well-mixed populations within $蠅$ Centauri's half-light radius </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Nitschai%2C+M+S">M. S. Nitschai</a>, <a href="/search/astro-ph?searchtype=author&query=Neumayer%2C+N">N. Neumayer</a>, <a href="/search/astro-ph?searchtype=author&query=H%C3%A4berle%2C+M">M. H盲berle</a>, <a href="/search/astro-ph?searchtype=author&query=Clontz%2C+C">C. Clontz</a>, <a href="/search/astro-ph?searchtype=author&query=Seth%2C+A+C">A. C. Seth</a>, <a href="/search/astro-ph?searchtype=author&query=Milone%2C+A+P">A. P. Milone</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro-Cuello%2C+M">M. Alfaro-Cuello</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">A. Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Dreizler%2C+S">S. Dreizler</a>, <a href="/search/astro-ph?searchtype=author&query=Feldmeier-Krause%2C+A">A. Feldmeier-Krause</a>, <a href="/search/astro-ph?searchtype=author&query=Husser%2C+T+-">T. -O. Husser</a>, <a href="/search/astro-ph?searchtype=author&query=Kacharov%2C+N">N. Kacharov</a>, <a href="/search/astro-ph?searchtype=author&query=Kamann%2C+S">S. Kamann</a>, <a href="/search/astro-ph?searchtype=author&query=Latour%2C+M">M. Latour</a>, <a href="/search/astro-ph?searchtype=author&query=Libralato%2C+M">M. Libralato</a>, <a href="/search/astro-ph?searchtype=author&query=van+de+Ven%2C+G">G. van de Ven</a>, <a href="/search/astro-ph?searchtype=author&query=Voggel%2C+K">K. Voggel</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Z">Z. Wang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.01688v2-abstract-short" style="display: inline;"> $蠅… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.01688v2-abstract-full').style.display = 'inline'; document.getElementById('2406.01688v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.01688v2-abstract-full" style="display: none;"> $蠅$ Centauri, the most massive globular cluster in the Milky Way, has long been suspected to be the stripped nucleus of a dwarf galaxy that fell into the Galaxy a long time ago. There is considerable evidence for this scenario including a large spread in metallicity and an unusually large number of distinct sub-populations seen in photometric studies. In this work, we use new MUSE spectroscopic and HST photometric catalogs to investigate the underlying metallicity distributions as well as the spatial variations of the populations within the cluster up to its half-light radius. Based on 11,050 member stars, the [M/H] distribution has a median of $ (-1.614 \pm 0.003)$ dex and a large spread of $\sim$ 1.37 dex reaching from $ -0.67$ dex to $ -2.04$ dex for 99.7 % of the stars. In addition, we show the chromosome map of the cluster, which separates the red giant branch stars into different sub-populations, and analyze the sub-populations of the metal-poorest component. Finally, we do not find any metallicity gradient within the half-light radius, and the different sub-populations are well mixed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.01688v2-abstract-full').style.display = 'none'; document.getElementById('2406.01688v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 18 figures, and 3 tables. Accepted for publication in ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 970, 152 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.06015">arXiv:2405.06015</a> <span> [<a href="https://arxiv.org/pdf/2405.06015">pdf</a>, <a href="https://arxiv.org/format/2405.06015">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1038/s41586-024-07511-z">10.1038/s41586-024-07511-z <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Fast-moving stars around an intermediate-mass black hole in Omega Centauri </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=H%C3%A4berle%2C+M">Maximilian H盲berle</a>, <a href="/search/astro-ph?searchtype=author&query=Neumayer%2C+N">Nadine Neumayer</a>, <a href="/search/astro-ph?searchtype=author&query=Seth%2C+A">Anil Seth</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">Andrea Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Libralato%2C+M">Mattia Libralato</a>, <a href="/search/astro-ph?searchtype=author&query=Baumgardt%2C+H">Holger Baumgardt</a>, <a href="/search/astro-ph?searchtype=author&query=Whitaker%2C+M">Matthew Whitaker</a>, <a href="/search/astro-ph?searchtype=author&query=Dumont%2C+A">Antoine Dumont</a>, <a href="/search/astro-ph?searchtype=author&query=Cuello%2C+M+A">Mayte Alfaro Cuello</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">Jay Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Clontz%2C+C">Callie Clontz</a>, <a href="/search/astro-ph?searchtype=author&query=Kacharov%2C+N">Nikolay Kacharov</a>, <a href="/search/astro-ph?searchtype=author&query=Kamann%2C+S">Sebastian Kamann</a>, <a href="/search/astro-ph?searchtype=author&query=Feldmeier-Krause%2C+A">Anja Feldmeier-Krause</a>, <a href="/search/astro-ph?searchtype=author&query=Milone%2C+A">Antonino Milone</a>, <a href="/search/astro-ph?searchtype=author&query=Nitschai%2C+M+S">Maria Selina Nitschai</a>, <a href="/search/astro-ph?searchtype=author&query=Pechetti%2C+R">Renuka Pechetti</a>, <a href="/search/astro-ph?searchtype=author&query=van+de+Ven%2C+G">Glenn van de Ven</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="2405.06015v2-abstract-short" style="display: inline;"> Black holes have been found over a wide range of masses, from stellar remnants with masses of 5-150 solar masses (Msun), to those found at the centers of galaxies with $M>10^5$ Msun. However, only a few debated candidate black holes exist between 150 and $10^5$ Msun. Determining the population of these intermediate-mass black holes is an important step towards understanding supermassive black hole… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.06015v2-abstract-full').style.display = 'inline'; document.getElementById('2405.06015v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.06015v2-abstract-full" style="display: none;"> Black holes have been found over a wide range of masses, from stellar remnants with masses of 5-150 solar masses (Msun), to those found at the centers of galaxies with $M>10^5$ Msun. However, only a few debated candidate black holes exist between 150 and $10^5$ Msun. Determining the population of these intermediate-mass black holes is an important step towards understanding supermassive black hole formation in the early universe. Several studies have claimed the detection of a central black hole in $蠅$ Centauri, the Milky Way's most massive globular cluster. However, these studies have been questioned due to the possible mass contribution of stellar mass black holes, their sensitivity to the cluster center, and the lack of fast-moving stars above the escape velocity. Here we report observations of seven fast-moving stars in the central 3 arcseconds (0.08 pc) of $蠅$ Centauri. The velocities of the fast-moving stars are significantly higher than the expected central escape velocity of the star cluster, so their presence can only be explained by being bound to a massive black hole. From the velocities alone, we can infer a firm lower limit of the black hole mass of $\sim$8,200 Msun, making this a compelling candidate for an intermediate-mass black hole in the local universe. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.06015v2-abstract-full').style.display = 'none'; document.getElementById('2405.06015v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">33 pages, 11 figures, and 2 tables. Published in Nature. This is the accepted author's version. The version of record is available from the Journal (open access)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nature 631, 285-288 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.01637">arXiv:2405.01637</a> <span> [<a href="https://arxiv.org/pdf/2405.01637">pdf</a>, <a href="https://arxiv.org/format/2405.01637">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The SDSS-V Local Volume Mapper (LVM): Scientific Motivation and Project Overview </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Drory%2C+N">Niv Drory</a>, <a href="/search/astro-ph?searchtype=author&query=Blanc%2C+G+A">Guillermo A. Blanc</a>, <a href="/search/astro-ph?searchtype=author&query=Kreckel%2C+K">Kathryn Kreckel</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez%2C+S+F">Sebastian F. Sanchez</a>, <a href="/search/astro-ph?searchtype=author&query=Mejia-Narvaez%2C+A">Alfredo Mejia-Narvaez</a>, <a href="/search/astro-ph?searchtype=author&query=Johnston%2C+E+J">Evelyn J. Johnston</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+A+M">Amy M. Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Pellegrini%2C+E+W">Eric W. Pellegrini</a>, <a href="/search/astro-ph?searchtype=author&query=Konidaris%2C+N+P">Nicholas P. Konidaris</a>, <a href="/search/astro-ph?searchtype=author&query=Herbst%2C+T">Tom Herbst</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez-Gallego%2C+J">Jose Sanchez-Gallego</a>, <a href="/search/astro-ph?searchtype=author&query=Kollmeier%2C+J+A">Juna A. Kollmeier</a>, <a href="/search/astro-ph?searchtype=author&query=de+Almeida%2C+F">Florence de Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Barrera-Ballesteros%2C+J+K">Jorge K. Barrera-Ballesteros</a>, <a href="/search/astro-ph?searchtype=author&query=Bizyaev%2C+D">Dmitry Bizyaev</a>, <a href="/search/astro-ph?searchtype=author&query=Brownstein%2C+J+R">Joel R. Brownstein</a>, <a href="/search/astro-ph?searchtype=author&query=Saguer%2C+M+C+i">Mar Canal i Saguer</a>, <a href="/search/astro-ph?searchtype=author&query=Cherinka%2C+B">Brian Cherinka</a>, <a href="/search/astro-ph?searchtype=author&query=Cioni%2C+M+L">Maria-Rosa L. Cioni</a>, <a href="/search/astro-ph?searchtype=author&query=Congiu%2C+E">Enrico Congiu</a>, <a href="/search/astro-ph?searchtype=author&query=Cosens%2C+M">Maren Cosens</a>, <a href="/search/astro-ph?searchtype=author&query=Dias%2C+B">Bruno Dias</a>, <a href="/search/astro-ph?searchtype=author&query=Donor%2C+J">John Donor</a>, <a href="/search/astro-ph?searchtype=author&query=Egorov%2C+O">Oleg Egorov</a>, <a href="/search/astro-ph?searchtype=author&query=Egorova%2C+E">Evgeniia Egorova</a> , et al. (26 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="2405.01637v1-abstract-short" style="display: inline;"> We present the Sloan Digital Sky Survey V (SDSS-V) Local Volume Mapper (LVM). The LVM is an integral-field spectroscopic survey of the Milky Way, Magellanic Clouds, and of a sample of local volume galaxies, connecting resolved pc-scale individual sources of feedback to kpc-scale ionized interstellar medium (ISM) properties. The 4-year survey covers the southern Milky Way disk at spatial resolution… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.01637v1-abstract-full').style.display = 'inline'; document.getElementById('2405.01637v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.01637v1-abstract-full" style="display: none;"> We present the Sloan Digital Sky Survey V (SDSS-V) Local Volume Mapper (LVM). The LVM is an integral-field spectroscopic survey of the Milky Way, Magellanic Clouds, and of a sample of local volume galaxies, connecting resolved pc-scale individual sources of feedback to kpc-scale ionized interstellar medium (ISM) properties. The 4-year survey covers the southern Milky Way disk at spatial resolutions of 0.05 to 1 pc, the Magellanic Clouds at 10 pc resolution, and nearby large galaxies at larger scales totaling $>4300$ square degrees of sky, and more than 55M spectra. It utilizes a new facility of alt-alt mounted siderostats feeding 16 cm refractive telescopes, lenslet-coupled fiber-optics, and spectrographs covering 3600-9800A at R ~ 4000. The ultra-wide field IFU has a diameter of 0.5 degrees with 1801 hexagonally packed fibers of 35.3 arcsec apertures. The siderostats allow for a completely stationary fiber system, avoiding instability of the line spread function seen in traditional fiber feeds. Scientifically, LVM resolves the regions where energy, momentum, and chemical elements are injected into the ISM at the scale of gas clouds, while simultaneously charting where energy is being dissipated (via cooling, shocks, turbulence, bulk flows, etc.) to global scales. This combined local and global view enables us to constrain physical processes regulating how stellar feedback operates and couples to galactic kinematics and disk-scale structures, such as the bar and spiral arms, as well as gas in- and out-flows. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.01637v1-abstract-full').style.display = 'none'; document.getElementById('2405.01637v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">29 pages, 12 figures, accepted for publication in The Astronomical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.03722">arXiv:2404.03722</a> <span> [<a href="https://arxiv.org/pdf/2404.03722">pdf</a>, <a href="https://arxiv.org/format/2404.03722">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ad47f5">10.3847/1538-4357/ad47f5 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> oMEGACat II -- Photometry and proper motions for 1.4 million stars in Omega Centauri and its rotation in the plane of the sky </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=H%C3%A4berle%2C+M">Maximilian H盲berle</a>, <a href="/search/astro-ph?searchtype=author&query=Neumayer%2C+N">Nadine Neumayer</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">Andrea Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Libralato%2C+M">Mattia Libralato</a>, <a href="/search/astro-ph?searchtype=author&query=Clontz%2C+C">Callie Clontz</a>, <a href="/search/astro-ph?searchtype=author&query=Seth%2C+A+C">Anil C. Seth</a>, <a href="/search/astro-ph?searchtype=author&query=Nitschai%2C+M+S">Maria Selina Nitschai</a>, <a href="/search/astro-ph?searchtype=author&query=Kamann%2C+S">Sebastian Kamann</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro-Cuello%2C+M">Mayte Alfaro-Cuello</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">Jay Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Dreizler%2C+S">Stefan Dreizler</a>, <a href="/search/astro-ph?searchtype=author&query=Feldmeier-Krause%2C+A">Anja Feldmeier-Krause</a>, <a href="/search/astro-ph?searchtype=author&query=Kacharov%2C+N">Nikolay Kacharov</a>, <a href="/search/astro-ph?searchtype=author&query=Latour%2C+M">Marilyn Latour</a>, <a href="/search/astro-ph?searchtype=author&query=Milone%2C+A">Antonino Milone</a>, <a href="/search/astro-ph?searchtype=author&query=Pechetti%2C+R">Renuka Pechetti</a>, <a href="/search/astro-ph?searchtype=author&query=van+de+Ven%2C+G">Glenn van de Ven</a>, <a href="/search/astro-ph?searchtype=author&query=Voggel%2C+K">Karina Voggel</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="2404.03722v2-abstract-short" style="display: inline;"> Omega Centauri ($蠅$ Cen) is the most massive globular cluster of the Milky Way. It is thought to be the nucleus of an accreted dwarf galaxy because of its high mass and its complex stellar populations. To decipher its formation history and study its dynamics, we created the most comprehensive kinematic catalog for its inner region, by analyzing both archival and new Hubble Space Telescope (HST) da… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03722v2-abstract-full').style.display = 'inline'; document.getElementById('2404.03722v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.03722v2-abstract-full" style="display: none;"> Omega Centauri ($蠅$ Cen) is the most massive globular cluster of the Milky Way. It is thought to be the nucleus of an accreted dwarf galaxy because of its high mass and its complex stellar populations. To decipher its formation history and study its dynamics, we created the most comprehensive kinematic catalog for its inner region, by analyzing both archival and new Hubble Space Telescope (HST) data. Our catalog contains 1 395 781 proper-motion measurements out to the half-light radius of the cluster ($\sim$5.0') and down to $m_{F625W}\approx$25. The typical baseline for our proper-motion measurements is 20 years, leading to a median 1D proper motion precision of $\sim$11 $渭$as yr$^{-1}$ for stars with $m_{F625W}\approx$18 mag, with even better precision ($\sim$6.6 $渭$as yr$^{-1}$) achieved in the extensively observed centermost (r$<$1.5') region. In addition to our astrometric measurements, we also obtained precise HST photometry in seven filters spanning from the ultraviolet to the near-infrared. This allows detailed color-magnitude-diagram studies and to separate the multiple stellar populations of the cluster. In this work, we describe the data reduction used to obtain both the photometric and the proper-motion measurements. We also illustrate the creation and the content of our catalog, which is made publicly available. Finally, we present measurements of the plane-of-sky rotation of $蠅$ Cen in the previously unprobed inner few arcminutes and a precise measurement of the inclination $i = (43.9\pm1.3)^\circ$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03722v2-abstract-full').style.display = 'none'; document.getElementById('2404.03722v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 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">43 pages, 25 figures, 9 tables. Published by ApJ. The full catalog is publicly available under: https://doi.org/10.5281/zenodo.11104046</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 970 192 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.02503">arXiv:2309.02503</a> <span> [<a href="https://arxiv.org/pdf/2309.02503">pdf</a>, <a href="https://arxiv.org/format/2309.02503">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/acf5db">10.3847/1538-4357/acf5db <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> oMEGACat I: MUSE spectroscopy of 300,000 stars within the half-light radius of $蠅$ Centauri </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Nitschai%2C+M+S">M. S. Nitschai</a>, <a href="/search/astro-ph?searchtype=author&query=Neumayer%2C+N">N. Neumayer</a>, <a href="/search/astro-ph?searchtype=author&query=Clontz%2C+C">C. Clontz</a>, <a href="/search/astro-ph?searchtype=author&query=H%C3%A4berle%2C+M">M. H盲berle</a>, <a href="/search/astro-ph?searchtype=author&query=Seth%2C+A+C">A. C. Seth</a>, <a href="/search/astro-ph?searchtype=author&query=Husser%2C+T+-">T. -O. Husser</a>, <a href="/search/astro-ph?searchtype=author&query=Kamann%2C+S">S. Kamann</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro-Cuello%2C+M">M. Alfaro-Cuello</a>, <a href="/search/astro-ph?searchtype=author&query=Kacharov%2C+N">N. Kacharov</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">A. Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Dotter%2C+A">A. Dotter</a>, <a href="/search/astro-ph?searchtype=author&query=Dreizler%2C+S">S. Dreizler</a>, <a href="/search/astro-ph?searchtype=author&query=Feldmeier-Krause%2C+A">A. Feldmeier-Krause</a>, <a href="/search/astro-ph?searchtype=author&query=Latour%2C+M">M. Latour</a>, <a href="/search/astro-ph?searchtype=author&query=Libralato%2C+M">M. Libralato</a>, <a href="/search/astro-ph?searchtype=author&query=Milone%2C+A+P">A. P. Milone</a>, <a href="/search/astro-ph?searchtype=author&query=Pechetti%2C+R">R. Pechetti</a>, <a href="/search/astro-ph?searchtype=author&query=van+de+Ven%2C+G">G. van de Ven</a>, <a href="/search/astro-ph?searchtype=author&query=Voggel%2C+K">K. Voggel</a>, <a href="/search/astro-ph?searchtype=author&query=Weisz%2C+D+R">Daniel R. Weisz</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.02503v2-abstract-short" style="display: inline;"> Omega Centauri ($蠅$ Cen) is the most massive globular cluster of the Milky Way and has been the focus of many studies that reveal the complexity of its stellar populations and kinematics. However, most previous studies have used photometric and spectroscopic datasets with limited spatial or magnitude coverage, while we aim to investigate it having full spatial coverage out to its half-light radius… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.02503v2-abstract-full').style.display = 'inline'; document.getElementById('2309.02503v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.02503v2-abstract-full" style="display: none;"> Omega Centauri ($蠅$ Cen) is the most massive globular cluster of the Milky Way and has been the focus of many studies that reveal the complexity of its stellar populations and kinematics. However, most previous studies have used photometric and spectroscopic datasets with limited spatial or magnitude coverage, while we aim to investigate it having full spatial coverage out to its half-light radius and stars ranging from the main sequence to the tip of the red giant branch. This is the first paper in a new survey of $蠅$ Cen that combines uniform imaging and spectroscopic data out to its half-light radius to study its stellar populations, kinematics, and formation history. In this paper, we present an unprecedented MUSE spectroscopic dataset combining 87 new MUSE pointings with previous observations collected from guaranteed time observations. We extract spectra of more than 300,000 stars reaching more than two magnitudes below the main sequence turn-off. We use these spectra to derive metallicity and line-of-sight velocity measurements and determine robust uncertainties on these quantities using repeat measurements. Applying quality cuts we achieve signal-to-noise ratios of 16.47/73.51 and mean metallicity errors of 0.174/0.031 dex for the main sequence stars (18 mag $\rm < mag_{F625W}<$22 mag) and red giant branch stars (16 mag $<\rm mag_{F625W}<$10 mag), respectively. We correct the metallicities for atomic diffusion and identify foreground stars. This massive spectroscopic dataset will enable future studies that will transform our understanding of $蠅$ Cen, allowing us to investigate the stellar populations, ages, and kinematics in great detail. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.02503v2-abstract-full').style.display = 'none'; document.getElementById('2309.02503v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">27 pages, 18 figures, 3 tables, published in ApJ, the catalog is available in the online material of the published article; typos corrected in this version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 958 8 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.05090">arXiv:2207.05090</a> <span> [<a href="https://arxiv.org/pdf/2207.05090">pdf</a>, <a href="https://arxiv.org/format/2207.05090">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1117/12.2629246">10.1117/12.2629246 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Validating the Local Volume Mapper acquisition and guiding hardware </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=H%C3%A4berle%2C+M">Maximilian H盲berle</a>, <a href="/search/astro-ph?searchtype=author&query=Herbst%2C+T+M">Thomas M. Herbst</a>, <a href="/search/astro-ph?searchtype=author&query=Bizenberger%2C+P">Peter Bizenberger</a>, <a href="/search/astro-ph?searchtype=author&query=Blanc%2C+G">Guillermo Blanc</a>, <a href="/search/astro-ph?searchtype=author&query=Briegel%2C+F">Florian Briegel</a>, <a href="/search/astro-ph?searchtype=author&query=Drory%2C+N">Niv Drory</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%A4ssler%2C+W">Wolfgang G盲ssler</a>, <a href="/search/astro-ph?searchtype=author&query=Konidaris%2C+N">Nick Konidaris</a>, <a href="/search/astro-ph?searchtype=author&query=Kreckel%2C+K">Kathryn Kreckel</a>, <a href="/search/astro-ph?searchtype=author&query=Kuhlberg%2C+M">Markus Kuhlberg</a>, <a href="/search/astro-ph?searchtype=author&query=Mohr%2C+L">Lars Mohr</a>, <a href="/search/astro-ph?searchtype=author&query=Pellegrini%2C+E">Eric Pellegrini</a>, <a href="/search/astro-ph?searchtype=author&query=Ramirez%2C+S">Solange Ramirez</a>, <a href="/search/astro-ph?searchtype=author&query=Ritz%2C+C">Christopher Ritz</a>, <a href="/search/astro-ph?searchtype=author&query=Rohloff%2C+R">Ralf-Rainer Rohloff</a>, <a href="/search/astro-ph?searchtype=author&query=St%C4%99pie%C5%84%2C+P">Paula St臋pie艅</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2207.05090v2-abstract-short" style="display: inline;"> The Local Volume Mapper (LVM) project is one of three surveys that form the Sloan Digital Sky Survey V. It will map the interstellar gas emission in a large fraction of the southern sky using wide-field integral field spectroscopy. Four 16-cm telescopes in siderostat configuration feed the integral field units (IFUs). A reliable acquisition and guiding (A&G) strategy will help ensure that we meet… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.05090v2-abstract-full').style.display = 'inline'; document.getElementById('2207.05090v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.05090v2-abstract-full" style="display: none;"> The Local Volume Mapper (LVM) project is one of three surveys that form the Sloan Digital Sky Survey V. It will map the interstellar gas emission in a large fraction of the southern sky using wide-field integral field spectroscopy. Four 16-cm telescopes in siderostat configuration feed the integral field units (IFUs). A reliable acquisition and guiding (A&G) strategy will help ensure that we meet our science goals. Each of the telescopes hosts commercial CMOS cameras used for A&G. In this work, we present our validation of the camera performance. Our tests show that the cameras have a readout noise of around 5.6e- and a dark current of 21e-/s, when operated at the ideal gain setting and at an ambient temperature of 20掳C. To ensure their performance at a high-altitude observing site, such as the Las Campanas Observatory, we studied the thermal behaviour of the cameras at different ambient pressures and with different passive cooling solutions. Using the measured properties, we calculated the brightness limit for guiding exposures. With a 5 s exposure time, we reach a depth of around 16.5 Gaia gmag with a signal-to-noise ratio (SNR)>5. Using Gaia Early Data Release 3, we verified that there are sufficient guide stars for each of the around 25000 survey pointings. For accurate acquisition, we also need to know the focal plane geometry. We present an approach that combines on-chip astrometry and using a point source microscope to measure the relative positions of the IFU lenslets and the individual CMOS pixels to around 2 $渭$m accuracy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.05090v2-abstract-full').style.display = 'none'; document.getElementById('2207.05090v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to SPIE Astronomical Telescopes + Instrumentation 2022, Ground-based and Airborne Instrumentation for Astronomy IX, Paper 12184-256</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> SPIE Proceedings Volume 12184, Ground-based and Airborne Instrumentation for Astronomy IX; 121846U (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2102.07782">arXiv:2102.07782</a> <span> [<a href="https://arxiv.org/pdf/2102.07782">pdf</a>, <a href="https://arxiv.org/format/2102.07782">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stab474">10.1093/mnras/stab474 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Hunting for intermediate-mass black holes in globular clusters: an astrometric study of NGC 6441 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=H%C3%A4berle%2C+M">Maximilian H盲berle</a>, <a href="/search/astro-ph?searchtype=author&query=Libralato%2C+M">Mattia Libralato</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">Andrea Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Watkins%2C+L+L">Laura L. Watkins</a>, <a href="/search/astro-ph?searchtype=author&query=Pott%2C+J">J枚rg-Uwe Pott</a>, <a href="/search/astro-ph?searchtype=author&query=Neumayer%2C+N">Nadine Neumayer</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Marel%2C+R+P">Roeland P. van der Marel</a>, <a href="/search/astro-ph?searchtype=author&query=Piotto%2C+G">Giampaolo Piotto</a>, <a href="/search/astro-ph?searchtype=author&query=Nardiello%2C+D">Domenico Nardiello</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="2102.07782v1-abstract-short" style="display: inline;"> We present an astrometric study of the proper motions (PMs) in the core of the globular cluster NGC 6441. The core of this cluster has a high density and observations with current instrumentation are very challenging. We combine ground-based, high-angular-resolution NACO@VLT images with Hubble Space Telescope ACS/HRC data and measure PMs with a temporal baseline of 15 yr for about 1400 stars in th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.07782v1-abstract-full').style.display = 'inline'; document.getElementById('2102.07782v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2102.07782v1-abstract-full" style="display: none;"> We present an astrometric study of the proper motions (PMs) in the core of the globular cluster NGC 6441. The core of this cluster has a high density and observations with current instrumentation are very challenging. We combine ground-based, high-angular-resolution NACO@VLT images with Hubble Space Telescope ACS/HRC data and measure PMs with a temporal baseline of 15 yr for about 1400 stars in the centermost 15 arcseconds of the cluster. We reach a PM precision of $\sim$30 $渭$as yr$^{-1}$ for bright, well-measured stars. Our results for the velocity dispersion are in good agreement with other studies and extend already-existing analyses of the stellar kinematics of NGC 6441 to its centermost region never probed before. In the innermost arcsecond of the cluster, we measure a velocity dispersion of (19.1 $\pm$ 2.0) km s$^{-1}$ for evolved stars. Because of its high mass, NGC 6441 is a promising candidate for harbouring an intermediate-mass black hole (IMBH). We combine our measurements with additional data from the literature and compute dynamical models of the cluster. We find an upper limit of $M_{\rm IMBH} < 1.32 \times 10^4\,\textrm{M}_\odot$ but we can neither confirm nor rule out its presence. We also refine the dynamical distance of the cluster to $12.74^{+0.16}_{-0.15}$ kpc. Although the hunt for an IMBH in NGC 6441 is not yet concluded, our results show how future observations with extremely-large telescopes will benefit from the long temporal baseline offered by existing high-angular-resolution data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.07782v1-abstract-full').style.display = 'none'; document.getElementById('2102.07782v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 12 figures, 2 tables. Accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2002.10017">arXiv:2002.10017</a> <span> [<a href="https://arxiv.org/pdf/2002.10017">pdf</a>, <a href="https://arxiv.org/format/2002.10017">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/ab7926">10.3847/1538-3881/ab7926 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> EDEN: Sensitivity Analysis and Transiting Planet Detection Limits for Nearby Late Red Dwarfs </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gibbs%2C+A">Aidan Gibbs</a>, <a href="/search/astro-ph?searchtype=author&query=Bixel%2C+A">Alex Bixel</a>, <a href="/search/astro-ph?searchtype=author&query=Rackham%2C+B">Benjamin Rackham</a>, <a href="/search/astro-ph?searchtype=author&query=Apai%2C+D">Daniel Apai</a>, <a href="/search/astro-ph?searchtype=author&query=Schlecker%2C+M">Martin Schlecker</a>, <a href="/search/astro-ph?searchtype=author&query=Espinoza%2C+N">Nestor Espinoza</a>, <a href="/search/astro-ph?searchtype=author&query=Mancini%2C+L">Luigi Mancini</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W">Wen-Ping Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Henning%2C+T">Thomas Henning</a>, <a href="/search/astro-ph?searchtype=author&query=Gabor%2C+P">Paul Gabor</a>, <a href="/search/astro-ph?searchtype=author&query=Boyle%2C+R">Richard Boyle</a>, <a href="/search/astro-ph?searchtype=author&query=Chavez%2C+J+P">Jose Perez Chavez</a>, <a href="/search/astro-ph?searchtype=author&query=Mousseau%2C+A">Allie Mousseau</a>, <a href="/search/astro-ph?searchtype=author&query=Dietrich%2C+J">Jeremy Dietrich</a>, <a href="/search/astro-ph?searchtype=author&query=Socia%2C+Q+J">Quentin Jay Socia</a>, <a href="/search/astro-ph?searchtype=author&query=Ip%2C+W">Wing Ip</a>, <a href="/search/astro-ph?searchtype=author&query=Ngeow%2C+C">Chow-Choong Ngeow</a>, <a href="/search/astro-ph?searchtype=author&query=Tsai%2C+A">Anli Tsai</a>, <a href="/search/astro-ph?searchtype=author&query=Bhandare%2C+A">Asmita Bhandare</a>, <a href="/search/astro-ph?searchtype=author&query=Marian%2C+V">Victor Marian</a>, <a href="/search/astro-ph?searchtype=author&query=Baehr%2C+H">Hans Baehr</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+S">Samantha Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Haberle%2C+M">Maximilian Haberle</a>, <a href="/search/astro-ph?searchtype=author&query=Keppler%2C+M">Miriam Keppler</a>, <a href="/search/astro-ph?searchtype=author&query=Molaverdikhani%2C+K">Karan Molaverdikhani</a> , et al. (1 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="2002.10017v1-abstract-short" style="display: inline;"> Small planets are common around late-M dwarfs and can be detected through highly precise photometry by the transit method. Planets orbiting nearby stars are particularly important as they are often the best-suited for future follow-up studies. We present observations of three nearby M-dwarfs referred to as EIC-1, EIC-2, and EIC-3, and use them to search for transits and set limits on the presence… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.10017v1-abstract-full').style.display = 'inline'; document.getElementById('2002.10017v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2002.10017v1-abstract-full" style="display: none;"> Small planets are common around late-M dwarfs and can be detected through highly precise photometry by the transit method. Planets orbiting nearby stars are particularly important as they are often the best-suited for future follow-up studies. We present observations of three nearby M-dwarfs referred to as EIC-1, EIC-2, and EIC-3, and use them to search for transits and set limits on the presence of planets. On most nights our observations are sensitive to Earth-sized transiting planets, and photometric precision is similar to or better than TESS for faint late-M dwarfs of the same magnitude (I=15 mag). We present our photometry and transit search pipeline, which utilizes simple median detrending in combination with transit least squares based transit detection (Hippke & Heller 2019).For these targets, and transiting planets between one and two Earth radii, we achieve an average transit detection probability of 60% between periods of 0.5 and 2 days, 30% between 2 and 5 days,and 10% between 5 and 10 days. These sensitivities are conservative compared to visual searches. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.10017v1-abstract-full').style.display = 'none'; document.getElementById('2002.10017v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 February, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1910.07014">arXiv:1910.07014</a> <span> [<a href="https://arxiv.org/pdf/1910.07014">pdf</a>, <a href="https://arxiv.org/ps/1910.07014">ps</a>, <a href="https://arxiv.org/format/1910.07014">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.icarus.2019.113495">10.1016/j.icarus.2019.113495 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Subsistence of ice-covered lakes during the Hesperian at Gale crater, Mars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kling%2C+A+M">Alexandre M. Kling</a>, <a href="/search/astro-ph?searchtype=author&query=Haberle%2C+R+M">Robert M. Haberle</a>, <a href="/search/astro-ph?searchtype=author&query=McKay%2C+C+P">Christopher P. McKay</a>, <a href="/search/astro-ph?searchtype=author&query=Bristow%2C+T+F">Thomas F. Bristow</a>, <a href="/search/astro-ph?searchtype=author&query=Rivera-Hernandez%2C+F">Frances Rivera-Hernandez</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="1910.07014v1-abstract-short" style="display: inline;"> Sedimentary deposits characterized by the Mars Science Laboratory Curiosity rover provide evidence that Gale crater, Mars intermittently hosted a fluvio-lacustrine environment during the Hesperian. However, estimates of the CO2 content of the atmosphere at the time the sediments in Gale crater were deposited are far less than needed by any climate model to maintain temperatures warm enough for sus… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.07014v1-abstract-full').style.display = 'inline'; document.getElementById('1910.07014v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1910.07014v1-abstract-full" style="display: none;"> Sedimentary deposits characterized by the Mars Science Laboratory Curiosity rover provide evidence that Gale crater, Mars intermittently hosted a fluvio-lacustrine environment during the Hesperian. However, estimates of the CO2 content of the atmosphere at the time the sediments in Gale crater were deposited are far less than needed by any climate model to maintain temperatures warm enough for sustained open water lake conditions due to the low solar energy input available at that time. We incrementally test the existence of open water conditions using energy balance calculations for the global, regional, and seasonal temperatures, and we assess if the preservation of liquid water was possible under perennial ice covers. We found scenarios where lacustrine conditions are preserved in a cold climate, where the resupply of water by the inflow of rivers and high precipitation rates are substituted by an abutting glacier. For equatorial temperatures as low as 240K-255K, the ice thickness ranges from 3-10 m, a value comparable to the range of those for the perennially ice-covered lakes in Antarctica (3-6 m). The ice-covered lake hypothesis is a compelling way to decouple the mineralogy and the climate by limiting the gas exchanges between the sediment and the CO2 atmosphere, and it eliminates the requirement for global mean temperatures above the freezing point. Not only do ice-covered lakes provide a baseline for exploring the range of possible lake scenarios for Gale crater during the Hesperian that is fully consistent with climate studies, but also they might have been ideal environments to sustain life on Mars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.07014v1-abstract-full').style.display = 'none'; document.getElementById('1910.07014v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 October, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2019. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1902.00738">arXiv:1902.00738</a> <span> [<a href="https://arxiv.org/pdf/1902.00738">pdf</a>, <a href="https://arxiv.org/format/1902.00738">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1538-3873/ab0c40">10.1088/1538-3873/ab0c40 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Development of the Warm Astrometric Mask for MICADO astrometry calibration </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rodeghiero%2C+G">Gabriele Rodeghiero</a>, <a href="/search/astro-ph?searchtype=author&query=Sawczuck%2C+M">Miriam Sawczuck</a>, <a href="/search/astro-ph?searchtype=author&query=Pott%2C+J+U">J枚rg Uwe Pott</a>, <a href="/search/astro-ph?searchtype=author&query=Gl%C3%BCck%2C+M">Martin Gl眉ck</a>, <a href="/search/astro-ph?searchtype=author&query=Biancalani%2C+E">Enrico Biancalani</a>, <a href="/search/astro-ph?searchtype=author&query=H%C3%A4berle%2C+M">Maximilian H盲berle</a>, <a href="/search/astro-ph?searchtype=author&query=Reichert%2C+H">Hannes Reichert</a>, <a href="/search/astro-ph?searchtype=author&query=Pernechele%2C+C">Claudio Pernechele</a>, <a href="/search/astro-ph?searchtype=author&query=Naranjo%2C+V">Vianak Naranjo</a>, <a href="/search/astro-ph?searchtype=author&query=Ventas%2C+J+M">Javier Moreno Ventas</a>, <a href="/search/astro-ph?searchtype=author&query=Bizenberger%2C+P">Peter Bizenberger</a>, <a href="/search/astro-ph?searchtype=author&query=Lessio%2C+L">Luigi Lessio</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="1902.00738v1-abstract-short" style="display: inline;"> The achievement of $渭$arcsec relative astrometry with ground-based, near infrared, extremely large telescopes requires a significant endeavour of calibration strategies. In this paper we address the removal of instrument optical distortions coming from the ELT first light instrument MICADO and its adaptive optics system MAORY by means of an astrometric calibration mask. The results of the test cam… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.00738v1-abstract-full').style.display = 'inline'; document.getElementById('1902.00738v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1902.00738v1-abstract-full" style="display: none;"> The achievement of $渭$arcsec relative astrometry with ground-based, near infrared, extremely large telescopes requires a significant endeavour of calibration strategies. In this paper we address the removal of instrument optical distortions coming from the ELT first light instrument MICADO and its adaptive optics system MAORY by means of an astrometric calibration mask. The results of the test campaign on a prototype mask (scale 1:2) has probed the manufacturing precision down to $\sim$ 50nm/1mm scale, leading to a relative precision $未蟽\sim 5e-5$. The assessed manufacturing precision indicates that an astrometric relative precision of $未蟽\sim 5e-5 = \frac{50渭as}{1 arcsec}$ is in principle achievable, disclosing $渭$arcsec near infrared astrometry behind an extremely large telescope. The impact of $\sim$ 10-100 nm error residuals on the mask pinholes position is tolerable at a calibration level as confirmed by ray tracing simulations of realistic MICADO distortion patterns affected by mid spatial frequencies residuals. We demonstrated that the MICADO astrometric precision of 50 $渭$as is achievable also in presence of a mid spatial frequencies pattern and manufacturing errors of the WAM by fitting the distorted WAM pattern seen through the instrument with a 10$^{th}$ order Legendre polynomial. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.00738v1-abstract-full').style.display = 'none'; document.getElementById('1902.00738v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 February, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2019. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1210.4216">arXiv:1210.4216</a> <span> [<a href="https://arxiv.org/pdf/1210.4216">pdf</a>, <a href="https://arxiv.org/ps/1210.4216">ps</a>, <a href="https://arxiv.org/format/1210.4216">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.icarus.2012.10.019">10.1016/j.icarus.2012.10.019 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> 3D modelling of the early Martian Climate under a denser CO2 atmosphere: Temperatures and CO2 ice clouds </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Forget%2C+F">Francois Forget</a>, <a href="/search/astro-ph?searchtype=author&query=Wordsworth%2C+R">Robin Wordsworth</a>, <a href="/search/astro-ph?searchtype=author&query=Millour%2C+E">Ehouarn Millour</a>, <a href="/search/astro-ph?searchtype=author&query=Madeleine%2C+J">Jean-Baptiste Madeleine</a>, <a href="/search/astro-ph?searchtype=author&query=Kerber%2C+L">Laura Kerber</a>, <a href="/search/astro-ph?searchtype=author&query=Leconte%2C+J">Jeremy Leconte</a>, <a href="/search/astro-ph?searchtype=author&query=Marcq%2C+E">Emmanuel Marcq</a>, <a href="/search/astro-ph?searchtype=author&query=Haberle%2C+R+M">Robert M. Haberle</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="1210.4216v1-abstract-short" style="display: inline;"> On the basis of geological evidence, it is often stated that the early martian climate was warm enough for liquid water to flow on the surface thanks to the greenhouse effect of a thick atmosphere. We present 3D global climate simulations of the early martian climate performed assuming a faint young sun and a CO2 atmosphere with pressure between 0.1 and 7 bars. The model includes a detailed radiat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1210.4216v1-abstract-full').style.display = 'inline'; document.getElementById('1210.4216v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1210.4216v1-abstract-full" style="display: none;"> On the basis of geological evidence, it is often stated that the early martian climate was warm enough for liquid water to flow on the surface thanks to the greenhouse effect of a thick atmosphere. We present 3D global climate simulations of the early martian climate performed assuming a faint young sun and a CO2 atmosphere with pressure between 0.1 and 7 bars. The model includes a detailed radiative transfer model using revised CO2 gas collision induced absorption properties, and a parameterisation of the CO2 ice cloud microphysical and radiative properties. A wide range of possible climates is explored by using various values of obliquities, orbital parameters, cloud microphysic parameters, atmospheric dust loading, and surface properties. Unlike on present day Mars, for pressures higher than a fraction of a bar, surface temperatures vary with altitude because of the adiabatic cooling and warming of the atmosphere when it moves vertically. In most simulations, CO2 ice clouds cover a major part of the planet but greenhouse effect does not exceed +15 K. We find that a CO2 atmosphere could not have raised the annual mean temperature above 0掳C anywhere on the planet. The collapse of the atmosphere into permanent CO2 ice caps is predicted for pressures higher than 3 bar, or conversely at pressure lower than one bar if the obliquity is low enough. Summertime diurnal mean surface temperatures above 0掳C (a condition which could have allowed rivers to form) are predicted for obliquity larger than 40掳 at high latitudes but not in locations where most valley networks are observed. In the absence of other warming mechanisms, our climate model results are thus consistent with a cold early Mars scenario in which non climatic mechanisms must occur to explain the evidence for liquid water. In a companion paper by Wordsworth et al., we simulate the hydrological cycle on such a planet. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1210.4216v1-abstract-full').style.display = 'none'; document.getElementById('1210.4216v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 October, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Icarus, In press. 23 pages, 18 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0609799">arXiv:astro-ph/0609799</a> <span>  </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/10.1089/ast.2006.0124">10.1089/ast.2006.0124 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Re-appraisal of the Habitability of Planets Around M Dwarf Stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Tarter%2C+J+C">Jill C. Tarter</a>, <a href="/search/astro-ph?searchtype=author&query=Backus%2C+P+R">Peter R. Backus</a>, <a href="/search/astro-ph?searchtype=author&query=Mancinelli%2C+R+L">Rocco L. Mancinelli</a>, <a href="/search/astro-ph?searchtype=author&query=Aurnou%2C+J+M">Jonathan M. Aurnou</a>, <a href="/search/astro-ph?searchtype=author&query=Backman%2C+D+E">Dana E. Backman</a>, <a href="/search/astro-ph?searchtype=author&query=Basri%2C+G+S">Gibor S. Basri</a>, <a href="/search/astro-ph?searchtype=author&query=Boss%2C+A+P">Alan P. Boss</a>, <a href="/search/astro-ph?searchtype=author&query=Clarke%2C+A">Andrew Clarke</a>, <a href="/search/astro-ph?searchtype=author&query=Deming%2C+D">Drake Deming</a>, <a href="/search/astro-ph?searchtype=author&query=Doyle%2C+L+R">Laurance R. Doyle</a>, <a href="/search/astro-ph?searchtype=author&query=Feigelson%2C+E+D">Eric D. Feigelson</a>, <a href="/search/astro-ph?searchtype=author&query=Freund%2C+F">Friedmann Freund</a>, <a href="/search/astro-ph?searchtype=author&query=Grinspoon%2C+D+H">David H. Grinspoon</a>, <a href="/search/astro-ph?searchtype=author&query=Haberle%2C+R+M">Robert M. Haberle</a>, <a href="/search/astro-ph?searchtype=author&query=Hauck%2C+S+A">Steven A. Hauck II</a>, <a href="/search/astro-ph?searchtype=author&query=Heath%2C+M+J">Martin J. Heath</a>, <a href="/search/astro-ph?searchtype=author&query=Henry%2C+T+J">Todd J. Henry</a>, <a href="/search/astro-ph?searchtype=author&query=Hollingsworth%2C+J+L">Jeffery L. Hollingsworth</a>, <a href="/search/astro-ph?searchtype=author&query=Joshi%2C+M+M">Manoj M. Joshi</a>, <a href="/search/astro-ph?searchtype=author&query=Kilston%2C+S">Steven Kilston</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+M+C">Michael C. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Meikle%2C+E">Eric Meikle</a>, <a href="/search/astro-ph?searchtype=author&query=Reid%2C+I+N">I. Neill Reid</a>, <a href="/search/astro-ph?searchtype=author&query=Rothschild%2C+L+J">Lynn J. Rothschild</a>, <a href="/search/astro-ph?searchtype=author&query=Scalo%2C+J+M">John M. Scalo</a> , et al. (7 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/0609799v2-abstract-short" style="display: inline;"> Stable, hydrogen-burning, M dwarf stars comprise about 75% of all stars in the Galaxy. They are extremely long-lived and because they are much smaller in mass than the Sun (between 0.5 and 0.08 MSun), their temperature and stellar luminosity are low and peaked in the red. We have re-examined what is known at present about the potential for a terrestrial planet forming within, or migrating into,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0609799v2-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0609799v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0609799v2-abstract-full" style="display: none;"> Stable, hydrogen-burning, M dwarf stars comprise about 75% of all stars in the Galaxy. They are extremely long-lived and because they are much smaller in mass than the Sun (between 0.5 and 0.08 MSun), their temperature and stellar luminosity are low and peaked in the red. We have re-examined what is known at present about the potential for a terrestrial planet forming within, or migrating into, the classic liquid-surface-water habitable zone close to an M dwarf star. Observations of protoplanetary disks suggest that planet-building materials are common around M dwarfs, but N-body simulations differ in their estimations of the likelihood of potentially-habitable, wet planets residing within their habitable zones, which are only ~ 1/5 to 1/50 of the width of that for a G star. Particularly in light of the claimed detection of the planets with masses as small as 5.5 and 7.5 MEarth orbiting M stars, there seems no reason to exclude the possibility of terrestrial planets. Tidally locked synchronous rotation within the narrow habitable zone doesn't necessarily lead to atmospheric collapse, and active stellar flaring may not be as much of an evolutionarily disadvantageous factor as has previously been supposed. We conclude that M dwarf stars may indeed be viable hosts for planets on which the origin and evolution of life can occur. A number of planetary processes such as cessation of geothermal activity, or thermal and non-thermal atmospheric loss processes may limit the duration of planetary habitability to periods far shorter than the extreme lifetime of the M dwarf star. Nevertheless, it makes sense to include M dwarf stars in programs that seek to find habitable worlds and evidence of life. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0609799v2-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0609799v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 November, 2006; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 September, 2006; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">To be published in Astrobiology. approx. 34 pages</span> </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: 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