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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/2501.10070">arXiv:2501.10070</a> <span> [<a href="https://arxiv.org/pdf/2501.10070">pdf</a>, <a href="https://arxiv.org/format/2501.10070">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> JWST Imaging of the Closest Globular Clusters -- V. The White Dwarfs Cooling Sequence of M4 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bedin%2C+L+R">L. R. Bedin</a>, <a href="/search/astro-ph?searchtype=author&query=Libralato%2C+M">M. Libralato</a>, <a href="/search/astro-ph?searchtype=author&query=Salaris%2C+M">M. Salaris</a>, <a href="/search/astro-ph?searchtype=author&query=Nardiello%2C+D">D. Nardiello</a>, <a href="/search/astro-ph?searchtype=author&query=Scalco%2C+M">M. Scalco</a>, <a href="/search/astro-ph?searchtype=author&query=Griggio%2C+M">M. Griggio</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Bergeron%2C+P">P. Bergeron</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">A. Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Gerasimov%2C+R">R. Gerasimov</a>, <a href="/search/astro-ph?searchtype=author&query=Burgasser%2C+A+J">A. J. Burgasser</a>, <a href="/search/astro-ph?searchtype=author&query=Apai%2C+D">D. Apai</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="2501.10070v1-abstract-short" style="display: inline;"> We combine infrared (IR) observations collected by the James Webb Space Telescope with optical deep images by the Hubble Space Telescope taken approximately 20 years earlier to compute proper-motion membership for the globular cluster (GC) M 4 (NGC 6121) along its entire white dwarf (WD) cooling sequence (CS). These new IR observations allow us, for only the second time in a GC, to compare WD mode… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.10070v1-abstract-full').style.display = 'inline'; document.getElementById('2501.10070v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.10070v1-abstract-full" style="display: none;"> We combine infrared (IR) observations collected by the James Webb Space Telescope with optical deep images by the Hubble Space Telescope taken approximately 20 years earlier to compute proper-motion membership for the globular cluster (GC) M 4 (NGC 6121) along its entire white dwarf (WD) cooling sequence (CS). These new IR observations allow us, for only the second time in a GC, to compare WD models with observations over a wide range of wavelengths, constraining fundamental astrophysical properties of WDs. Furthermore, we investigate the presence of WDs with IR excess along the WD CS of M 4, similar to the recent study conducted on the GC NGC 6397. We also determine the age difference between M 4 and NGC 6397 by comparing the absolute F150W2 magnitudes of the luminosity function peak at the bottom of the observed WD CS, and find that M 4 is slightly younger, by 0.8+/-0.5 Gyr. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.10070v1-abstract-full').style.display = 'none'; document.getElementById('2501.10070v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </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, 7 figures. Accepted for publication on Astronomische Nachrichten on 15th Jan 2025. Manuscript ID: ASNA.20240125</span> </p> </li> <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/2411.11978">arXiv:2411.11978</a> <span> [<a href="https://arxiv.org/pdf/2411.11978">pdf</a>, <a href="https://arxiv.org/format/2411.11978">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> <p class="title is-5 mathjax"> STIPS: The Nancy Grace Roman Space Telescope Imaging Product Simulator </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=STIPS+Development+Team"> STIPS Development Team</a>, <a href="/search/astro-ph?searchtype=author&query=Gomez%2C+S">Sebastian Gomez</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">Andrea Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Al-Kowsi%2C+H">Hanna Al-Kowsi</a>, <a href="/search/astro-ph?searchtype=author&query=Desjardins%2C+T">Tyler Desjardins</a>, <a href="/search/astro-ph?searchtype=author&query=Geda%2C+R">Robel Geda</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+E">Eunkyu Han</a>, <a href="/search/astro-ph?searchtype=author&query=Otor%2C+O+J">O. Justin Otor</a>, <a href="/search/astro-ph?searchtype=author&query=Riedel%2C+A">Adric Riedel</a>, <a href="/search/astro-ph?searchtype=author&query=Ryan%2C+R">Russell Ryan</a>, <a href="/search/astro-ph?searchtype=author&query=Spitzer%2C+I">Isaac Spitzer</a>, <a href="/search/astro-ph?searchtype=author&query=York%2C+B">Brian York</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="2411.11978v1-abstract-short" style="display: inline;"> The Space Telescope Imaging Product Simulator (STIPS) is a Python-based package that can be used to simulate scenes from the upcoming \textit{Nancy Grace Roman Space Telescope} (\nancy). STIPS is able to generate post-pipeline astronomical images of any number of sensor chip assembly (SCA) detectors, up to the entire 18-SCA Wide-Field Instrument array on \nancy. STIPS can inject either point sprea… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.11978v1-abstract-full').style.display = 'inline'; document.getElementById('2411.11978v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.11978v1-abstract-full" style="display: none;"> The Space Telescope Imaging Product Simulator (STIPS) is a Python-based package that can be used to simulate scenes from the upcoming \textit{Nancy Grace Roman Space Telescope} (\nancy). STIPS is able to generate post-pipeline astronomical images of any number of sensor chip assembly (SCA) detectors, up to the entire 18-SCA Wide-Field Instrument array on \nancy. STIPS can inject either point spread functions generated with {\tt WebbPSF}, or extended sources in any of the \nancy filters. The output images can include flat field, dark current, and cosmic ray residuals. Additionally, STIPS includes an estimate of Poisson and readout noise, as well as an estimate of the zodiacal background and internal background from the telescope. However, STIPS does not include instrument saturation, non-linearity, or distortion effects. STIPS is provided as an open source repository on GitHub. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.11978v1-abstract-full').style.display = 'none'; document.getElementById('2411.11978v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to PASP. 10 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/2410.12968">arXiv:2410.12968</a> <span> [<a href="https://arxiv.org/pdf/2410.12968">pdf</a>, <a href="https://arxiv.org/format/2410.12968">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/10.1093/mnras/stae2222">10.1093/mnras/stae2222 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Energy equipartition in multiple-population globular clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Livernois%2C+A+R">A. R. Livernois</a>, <a href="/search/astro-ph?searchtype=author&query=Aros%2C+F+I">F. I. Aros</a>, <a href="/search/astro-ph?searchtype=author&query=Vesperini%2C+E">E. Vesperini</a>, <a href="/search/astro-ph?searchtype=author&query=Askar%2C+A">A. Askar</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">A. Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Giersz%2C+M">M. Giersz</a>, <a href="/search/astro-ph?searchtype=author&query=Hong%2C+J">J. Hong</a>, <a href="/search/astro-ph?searchtype=author&query=Hypki%2C+A">A. Hypki</a>, <a href="/search/astro-ph?searchtype=author&query=Libralato%2C+M">M. Libralato</a>, <a href="/search/astro-ph?searchtype=author&query=Ziliotto%2C+T">T. Ziliotto</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.12968v1-abstract-short" style="display: inline;"> We present the results of Monte Carlo simulations aimed at exploring the evolution towards energy equipartition of first- (1G) and second-generation (2G) stars in multiple-population globular clusters and how this evolution is affected by the initial differences between the spatial distributions of the two populations. Our results show that these initial differences have fundamental implications f… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.12968v1-abstract-full').style.display = 'inline'; document.getElementById('2410.12968v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.12968v1-abstract-full" style="display: none;"> We present the results of Monte Carlo simulations aimed at exploring the evolution towards energy equipartition of first- (1G) and second-generation (2G) stars in multiple-population globular clusters and how this evolution is affected by the initial differences between the spatial distributions of the two populations. Our results show that these initial differences have fundamental implications for the evolution towards energy equipartition of the two populations. We find that 2G stars, which are assumed to be initially more centrally concentrated than 1G stars, are generally characterized by a more rapid evolution towards energy equipartition. The evolution towards energy equipartition depends on the velocity dispersion component and is more rapid for the tangential velocity dispersion. The extent of the present-day differences between the degree of energy equipartition of 2G and 1G stars depends on the cluster's dynamical age and may be more significant in the tangential velocity dispersion and at intermediate distances from the cluster's center around the half-mass radius. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.12968v1-abstract-full').style.display = 'none'; document.getElementById('2410.12968v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 13 figures, Published in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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/2409.06774">arXiv:2409.06774</a> <span> [<a href="https://arxiv.org/pdf/2409.06774">pdf</a>, <a href="https://arxiv.org/format/2409.06774">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> JWST imaging of the closest globular clusters -- IV. Chemistry, luminosity, and mass functions of the lowest-mass members in the NIRISS parallel fields </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Libralato%2C+M">M. Libralato</a>, <a href="/search/astro-ph?searchtype=author&query=Gerasimov%2C+R">R. Gerasimov</a>, <a href="/search/astro-ph?searchtype=author&query=Bedin%2C+L">L. Bedin</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Apai%2C+D">D. Apai</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">A. Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Burgasser%2C+A+J">A. J. Burgasser</a>, <a href="/search/astro-ph?searchtype=author&query=Griggio%2C+M">M. Griggio</a>, <a href="/search/astro-ph?searchtype=author&query=Nardiello%2C+D">D. Nardiello</a>, <a href="/search/astro-ph?searchtype=author&query=Salaris%2C+M">M. Salaris</a>, <a href="/search/astro-ph?searchtype=author&query=Scalco%2C+M">M. Scalco</a>, <a href="/search/astro-ph?searchtype=author&query=Vesperini%2C+E">E. Vesperini</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="2409.06774v1-abstract-short" style="display: inline;"> We present observations of the two closest globular clusters, NGC 6121 and NGC 6397, taken with the NIRISS detector of JWST. The combination of our new JWST data with archival Hubble Space Telescope (HST) images allows us to compute proper motions, disentangle cluster members from field objects, and probe the main sequence (MS) of the clusters down to <0.1 $M_\odot$ as well as the brighter part of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.06774v1-abstract-full').style.display = 'inline'; document.getElementById('2409.06774v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.06774v1-abstract-full" style="display: none;"> We present observations of the two closest globular clusters, NGC 6121 and NGC 6397, taken with the NIRISS detector of JWST. The combination of our new JWST data with archival Hubble Space Telescope (HST) images allows us to compute proper motions, disentangle cluster members from field objects, and probe the main sequence (MS) of the clusters down to <0.1 $M_\odot$ as well as the brighter part of the white-dwarf sequence. We show that theoretical isochrones fall short in modeling the low-mass MS and discuss possible explanations for the observed discrepancies. Our analysis suggests that the lowest-mass members of both clusters are significantly more metal-rich and oxygen-poor than their higher-mass counterparts. It is unclear whether the difference is caused by a genuine mass-dependent chemical heterogeneity, low-temperature atmospheric processes altering the observed abundances, or systematic shortcomings in the models. We computed the present-day local luminosity and mass functions of the two clusters; our data reveal a strong flattening of the mass function indicative of a significant preferential loss of low-mass stars in agreement with previous dynamical models for these two clusters. We have made our NIRISS astro-photometric catalogs and stacked images publicly available to the community. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.06774v1-abstract-full').style.display = 'none'; document.getElementById('2409.06774v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 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">15 pages, 12 figures, 2 tables. Accepted for publication in A&A on September 04, 2024. Astro-photometric catalogs and stacked images will be available at the CDS after the paper will be published</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.04533">arXiv:2409.04533</a> <span> [<a href="https://arxiv.org/pdf/2409.04533">pdf</a>, <a href="https://arxiv.org/format/2409.04533">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> The HST Large Programme on Omega Centauri -- VII. The white dwarf cooling sequence </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Scalco%2C+M">M. Scalco</a>, <a href="/search/astro-ph?searchtype=author&query=Salaris%2C+M">M. Salaris</a>, <a href="/search/astro-ph?searchtype=author&query=Bedin%2C+L">L. Bedin</a>, <a href="/search/astro-ph?searchtype=author&query=Griggio%2C+M">M. Griggio</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=Nardiello%2C+D">D. Nardiello</a>, <a href="/search/astro-ph?searchtype=author&query=Vesperini%2C+E">E. Vesperini</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Bergeron%2C+P">P. Bergeron</a>, <a href="/search/astro-ph?searchtype=author&query=Burgasser%2C+A">A. Burgasser</a>, <a href="/search/astro-ph?searchtype=author&query=Apai%2C+D">D. Apai</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="2409.04533v1-abstract-short" style="display: inline;"> We present a study of the white dwarf (WD) cooling sequence (CS) in the globular cluster (GC) Omega Centauri, the primary goal of a dedicated Hubble Space Telescope (HST) programme. Our analysis has revealed that the peak at the termination of the WD CS is located at $m_{\rm F606W}$=30.1$\pm$0.2 (equivalent to $V$$\sim$31). The brighter part of Omega Centauri's WD CS is consistent with the presenc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.04533v1-abstract-full').style.display = 'inline'; document.getElementById('2409.04533v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.04533v1-abstract-full" style="display: none;"> We present a study of the white dwarf (WD) cooling sequence (CS) in the globular cluster (GC) Omega Centauri, the primary goal of a dedicated Hubble Space Telescope (HST) programme. Our analysis has revealed that the peak at the termination of the WD CS is located at $m_{\rm F606W}$=30.1$\pm$0.2 (equivalent to $V$$\sim$31). The brighter part of Omega Centauri's WD CS is consistent with the presence of massive He-core WDs, in agreement with previous HST analyses with ultraviolet and blue filters. Comparative analyses of the WD luminosity function (LF) with theoretical counterparts have shown that a single-age population for the cluster is compatible with the data. However, an analysis of just the WD LF cannot entirely exclude the possibility of an age range, due to uncertainties in the present-day WD mass function, with a star formation history potentially spanning up to 5 billion years, predominantly comprising stars about 13 Gyr old, and with just a minority potentially as young as 8 Gyr. This underscores the need for global spectroscopic and photometric investigations that include simultaneously the WD populations together with the previous evolutionary phases to fully understand the cluster's diverse chemical compositions and ages. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.04533v1-abstract-full').style.display = 'none'; document.getElementById('2409.04533v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 September, 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">10 pages, 9 figures. Accepted for publication in Astronomy & Astrophysics on Sep 5, 2024</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.18135">arXiv:2407.18135</a> <span> [<a href="https://arxiv.org/pdf/2407.18135">pdf</a>, <a href="https://arxiv.org/format/2407.18135">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Testing Cluster Membership of Planetary Nebulae with High-Precision Proper Motions. I. HST Observations of JaFu 1 Near the Globular Cluster Palomar 6 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bond%2C+H+E">Howard E. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">Andrea Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Sahu%2C+K+C">Kailash C. Sahu</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.18135v1-abstract-short" style="display: inline;"> If a planetary nebula (PN) is shown to be a member of a star cluster, we obtain important new constraints on the mass and chemical composition of the PN's progenitor star, which cannot be determined for PNe in the field. Cluster membership can be tested by requiring the projected separation between the PN and cluster to be within the tidal radius of the cluster, and the objects to have nearly iden… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.18135v1-abstract-full').style.display = 'inline'; document.getElementById('2407.18135v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.18135v1-abstract-full" style="display: none;"> If a planetary nebula (PN) is shown to be a member of a star cluster, we obtain important new constraints on the mass and chemical composition of the PN's progenitor star, which cannot be determined for PNe in the field. Cluster membership can be tested by requiring the projected separation between the PN and cluster to be within the tidal radius of the cluster, and the objects to have nearly identical radial velocities (RVs) and interstellar extinctions, and nearly identical proper motions (PMs). In an earlier study, we used PMs to confirm that three PNe, which had already passed the other tests, are highly likely to be members of Galactic globular clusters (GCs). For a fourth object, the PN JaFu 1, which lies in the Galactic bulge near the GC Palomar 6 on the sky and has a similar RV, the available PM measurement gave equivocal results. We have now obtained new high-resolution images of the central star of JaFu 1 with the Hubble Space Telescope (HST) which, combined with archival HST frames taken 14 and 16 years earlier, provide a high-precision PM. Unfortunately, we find that the PM of the central star differs from that of the cluster with high statistical significance, and thus is unlikely to be a member of Palomar 6. Nevertheless, JaFu 1 is of astrophysical interest because its nucleus appears to be a member of the rare class of "EGB 6-type" central stars, which are associated with compact emission-line knots. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.18135v1-abstract-full').style.display = 'none'; document.getElementById('2407.18135v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted by 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/2407.07769">arXiv:2407.07769</a> <span> [<a href="https://arxiv.org/pdf/2407.07769">pdf</a>, <a href="https://arxiv.org/format/2407.07769">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ad571c">10.3847/1538-4357/ad571c <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> HSTPROMO Internal Proper Motion Kinematics of Dwarf Spheroidal Galaxies: I. Velocity Anisotropy and Dark Matter Cusp Slope of Draco </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vitral%2C+E">Eduardo Vitral</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=Sohn%2C+S+T">Sangmo Tony Sohn</a>, <a href="/search/astro-ph?searchtype=author&query=Libralato%2C+M">Mattia Libralato</a>, <a href="/search/astro-ph?searchtype=author&query=del+Pino%2C+A">Andr茅s del Pino</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=Bellini%2C+A">Andrea Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Walker%2C+M+G">Matthew G. Walker</a>, <a href="/search/astro-ph?searchtype=author&query=Besla%2C+G">Gurtina Besla</a>, <a href="/search/astro-ph?searchtype=author&query=Pawlowski%2C+M+S">Marcel S. Pawlowski</a>, <a href="/search/astro-ph?searchtype=author&query=Mamon%2C+G+A">Gary A. Mamon</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.07769v1-abstract-short" style="display: inline;"> We analyze four epochs of HST imaging over 18 years for the Draco dwarf spheroidal galaxy. We measure precise proper motions (PMs) for hundreds of stars and combine these with existing line-of-sight (LOS) velocities. This provides the first radially-resolved 3D velocity dispersion profiles for any dwarf galaxy. These constrain the intrinsic velocity anisotropy and resolve the mass-anisotropy degen… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.07769v1-abstract-full').style.display = 'inline'; document.getElementById('2407.07769v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.07769v1-abstract-full" style="display: none;"> We analyze four epochs of HST imaging over 18 years for the Draco dwarf spheroidal galaxy. We measure precise proper motions (PMs) for hundreds of stars and combine these with existing line-of-sight (LOS) velocities. This provides the first radially-resolved 3D velocity dispersion profiles for any dwarf galaxy. These constrain the intrinsic velocity anisotropy and resolve the mass-anisotropy degeneracy. We solve the Jeans equations in oblate axisymmetric geometry to infer the mass profile. We find the velocity dispersion to be radially anisotropic along the symmetry axis and tangentially anisotropic in the equatorial plane, with a globally-averaged value $\overline{尾_{\mathrm B}}=-0.20^{+ 0.28}_{- 0.53}$, (where $1 - 尾_{\mathrm B} \equiv \langle v_{\mathrm{ tan}}^2 \rangle / \langle v_{\mathrm{ rad}}^2 \rangle$ in 3D). The logarithmic dark matter (DM) density slope over the observed radial range, $螕_{\mathrm{ dark}}$, is $-0.83^{+ 0.32}_{- 0.37}$, consistent with the inner cusp predicted in $螞$CDM cosmology. As expected given Draco's low mass and ancient star formation history, it does not appear to have been dissolved by baryonic processes. We rule out cores larger than 487, 717, 942 pc at respective 1-, 2-, 3-$蟽$ confidence, thus imposing important constraints on the self-interacting DM cross-section. Spherical models yield biased estimates for both the velocity anisotropy and the inferred slope. The circular velocity at our outermost data point (900 pc) is $24.19^{+ 6.31}_{- 2.97} \ \mathrm{km~s^{-1}}s$. We infer a dynamical distance of $75.37^{+ 4.73}_{- 4.00}$ kpc, and show that Draco has a modest LOS rotation, with $\left<v / 蟽\right> = 0.22 \pm 0.09$. Our results provide a new stringent test of the so-called `cusp-core' problem that can be readily extended to other dwarfs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.07769v1-abstract-full').style.display = 'none'; document.getElementById('2407.07769v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">35 pages, 18 figures, 3 Tables. Accepted for publication in ApJ. Journal version has better readability. Data is available at Zenodo: https://zenodo.org/records/11111113</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal, 970:1 (26pp), 2024 July 20 </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/2406.16646">arXiv:2406.16646</a> <span> [<a href="https://arxiv.org/pdf/2406.16646">pdf</a>, <a href="https://arxiv.org/format/2406.16646">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202450584">10.1051/0004-6361/202450584 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The VISTA Variables in the V铆a L谩ctea eXtended (VVVX) ESO public survey: Completion of the observations and legacy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Saito%2C+R+K">R. K. Saito</a>, <a href="/search/astro-ph?searchtype=author&query=Hempel%2C+M">M. Hempel</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso-Garc%C3%ADa%2C+J">J. Alonso-Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+P+W">P. W. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso%2C+S">S. Alonso</a>, <a href="/search/astro-ph?searchtype=author&query=Baravalle%2C+L">L. Baravalle</a>, <a href="/search/astro-ph?searchtype=author&query=Borissova%2C+J">J. Borissova</a>, <a href="/search/astro-ph?searchtype=author&query=Caceres%2C+C">C. Caceres</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%C3%A9%2C+A+N">A. N. Chen茅</a>, <a href="/search/astro-ph?searchtype=author&query=Cross%2C+N+J+G">N. J. G. Cross</a>, <a href="/search/astro-ph?searchtype=author&query=Duplancic%2C+F">F. Duplancic</a>, <a href="/search/astro-ph?searchtype=author&query=Garro%2C+E+R">E. R. Garro</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%B3mez%2C+M">M. G贸mez</a>, <a href="/search/astro-ph?searchtype=author&query=Ivanov%2C+V+D">V. D. Ivanov</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtev%2C+R">R. Kurtev</a>, <a href="/search/astro-ph?searchtype=author&query=Luna%2C+A">A. Luna</a>, <a href="/search/astro-ph?searchtype=author&query=Majaess%2C+D">D. Majaess</a>, <a href="/search/astro-ph?searchtype=author&query=Navarro%2C+M+G">M. G. Navarro</a>, <a href="/search/astro-ph?searchtype=author&query=Pullen%2C+J+B">J. B. Pullen</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">M. Rejkuba</a>, <a href="/search/astro-ph?searchtype=author&query=Sanders%2C+J+L">J. L. Sanders</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+L+C">L. C. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Albino%2C+P+H+C">P. H. C. Albino</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso%2C+M+V">M. V. Alonso</a> , et al. (121 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.16646v1-abstract-short" style="display: inline;"> The ESO public survey VISTA Variables in the V铆a L谩ctea (VVV) surveyed the inner Galactic bulge and the adjacent southern Galactic disk from $2009-2015$. Upon its conclusion, the complementary VVV eXtended (VVVX) survey has expanded both the temporal as well as spatial coverage of the original VVV area, widening it from $562$ to $1700$ sq. deg., as well as providing additional epochs in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.16646v1-abstract-full').style.display = 'inline'; document.getElementById('2406.16646v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.16646v1-abstract-full" style="display: none;"> The ESO public survey VISTA Variables in the V铆a L谩ctea (VVV) surveyed the inner Galactic bulge and the adjacent southern Galactic disk from $2009-2015$. Upon its conclusion, the complementary VVV eXtended (VVVX) survey has expanded both the temporal as well as spatial coverage of the original VVV area, widening it from $562$ to $1700$ sq. deg., as well as providing additional epochs in $JHK_{\rm s}$ filters from $2016-2023$. With the completion of VVVX observations during the first semester of 2023, we present here the observing strategy, a description of data quality and access, and the legacy of VVVX. VVVX took $\sim 2000$ hours, covering about 4% of the sky in the bulge and southern disk. VVVX covered most of the gaps left between the VVV and the VISTA Hemisphere Survey (VHS) areas and extended the VVV time baseline in the obscured regions affected by high extinction and hence hidden from optical observations. VVVX provides a deep $JHK_{\rm s}$ catalogue of $\gtrsim 1.5\times10^9$ point sources, as well as a $K_{\rm s}$ band catalogue of $\sim 10^7$ variable sources. Within the existing VVV area, we produced a $5D$ map of the surveyed region by combining positions, distances, and proper motions of well-understood distance indicators such as red clump stars, RR Lyrae, and Cepheid variables. In March 2023 we successfully finished the VVVX survey observations that started in 2016, an accomplishment for ESO Paranal Observatory upon 4200 hours of observations for VVV+VVVX. The VVV+VVVX catalogues complement those from the Gaia mission at low Galactic latitudes and provide spectroscopic targets for the forthcoming ESO high-multiplex spectrographs MOONS and 4MOST. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.16646v1-abstract-full').style.display = 'none'; document.getElementById('2406.16646v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 June, 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">17 pages, 11 figures (+ appendix). Accepted for publication in Astronomy and Astrophysics in section 14: Catalogs and data</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 689, A148 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.01688">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/2405.01635">arXiv:2405.01635</a> <span> [<a href="https://arxiv.org/pdf/2405.01635">pdf</a>, <a href="https://arxiv.org/format/2405.01635">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> JWST Imaging of the Closest Globular Clusters -- III. Multiple Populations along the low-mass Main Sequence stars of NGC 6397 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Scalco%2C+M">M. Scalco</a>, <a href="/search/astro-ph?searchtype=author&query=Libralato%2C+M">M. Libralato</a>, <a href="/search/astro-ph?searchtype=author&query=Gerasimov%2C+R">R. Gerasimov</a>, <a href="/search/astro-ph?searchtype=author&query=Bedin%2C+L+R">L. R. Bedin</a>, <a href="/search/astro-ph?searchtype=author&query=Vesperini%2C+E">E. Vesperini</a>, <a href="/search/astro-ph?searchtype=author&query=Nardiello%2C+D">D. Nardiello</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">A. Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Griggio%2C+M">M. Griggio</a>, <a href="/search/astro-ph?searchtype=author&query=Apai%2C+D">D. Apai</a>, <a href="/search/astro-ph?searchtype=author&query=Salaris%2C+M">M. Salaris</a>, <a href="/search/astro-ph?searchtype=author&query=Burgasser%2C+A">A. Burgasser</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">J. Anderson</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="2405.01635v2-abstract-short" style="display: inline;"> Thanks to its exceptional near-infrared photometry, JWST can effectively contribute to the discovery, characterization, and understanding of multiple stellar populations in globular clusters, especially at low masses where the Hubble Space Telescope (HST) faces limitations. This paper continues the efforts of the JWST GO-1979 program in exploring the faintest members of the globular cluster NGC 63… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.01635v2-abstract-full').style.display = 'inline'; document.getElementById('2405.01635v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.01635v2-abstract-full" style="display: none;"> Thanks to its exceptional near-infrared photometry, JWST can effectively contribute to the discovery, characterization, and understanding of multiple stellar populations in globular clusters, especially at low masses where the Hubble Space Telescope (HST) faces limitations. This paper continues the efforts of the JWST GO-1979 program in exploring the faintest members of the globular cluster NGC 6397. Here we show that the combination of HST and JWST data allows us to identify two groups of MS stars (MSa, the first-generation, and MSb, the second-generation group). We measured the ratio between the two groups and combined it with measurements from the literature focused on more central fields and more massive stars compared to our study. We find that the MSa and MSb stars are present in a $\approx$30-70 ratio regardless of the distance from the centre of the cluster and the mass of the stars used so far. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.01635v2-abstract-full').style.display = 'none'; document.getElementById('2405.01635v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 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">7 pages, 6 figures, 1 table, A&A accepted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.01631">arXiv:2405.01631</a> <span> [<a href="https://arxiv.org/pdf/2405.01631">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> JWST Imaging of the Closest Globular Clusters -- I. Possible Infrared Excess Among White Dwarfs in NGC 6397 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bedin%2C+L+R">L. R. Bedin</a>, <a href="/search/astro-ph?searchtype=author&query=Nardiello%2C+D">D. Nardiello</a>, <a href="/search/astro-ph?searchtype=author&query=Salaris%2C+M">M. Salaris</a>, <a href="/search/astro-ph?searchtype=author&query=Libralato%2C+M">M. Libralato</a>, <a href="/search/astro-ph?searchtype=author&query=Bergeron%2C+P">P. Bergeron</a>, <a href="/search/astro-ph?searchtype=author&query=Burgasser%2C+A+J">A. J. Burgasser</a>, <a href="/search/astro-ph?searchtype=author&query=Apai%2C+D">D. Apai</a>, <a href="/search/astro-ph?searchtype=author&query=Griggio%2C+M">M. Griggio</a>, <a href="/search/astro-ph?searchtype=author&query=Scalco%2C+M">M. Scalco</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Gerasimov%2C+R">R. Gerasimov</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">A. Bellini</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="2405.01631v1-abstract-short" style="display: inline;"> We present James Webb Space Telescope observations of the globular cluster NGC 6397 and use them to extend to infrared wavelengths the characterization of the cluster's entire white dwarf (WD) cooling sequence (CS). The data allows us to probe fundamental astrophysical WD properties and to search for evidence in their colors for (or against) the existence of ancient planetary systems. The existing… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.01631v1-abstract-full').style.display = 'inline'; document.getElementById('2405.01631v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.01631v1-abstract-full" style="display: none;"> We present James Webb Space Telescope observations of the globular cluster NGC 6397 and use them to extend to infrared wavelengths the characterization of the cluster's entire white dwarf (WD) cooling sequence (CS). The data allows us to probe fundamental astrophysical WD properties and to search for evidence in their colors for (or against) the existence of ancient planetary systems. The existing archival Hubble Space Telescope imaging data obtained ~18 years ago reach ultra-deep optical magnitudes (V~31) and allow us to derive a near-perfect separation between field and cluster members. We detect an apparent split in the lower part of the WD CS of NGC 6397. The red part of the WD CS, containing about 25% of the total, exhibits significant IR-excess of up to Delta m_F322W2 ~ 0.5 mag. These infrared excesses require both theoretical and observational follow-ups to confirm their veracity and to ascertain their true nature. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.01631v1-abstract-full').style.display = 'none'; document.getElementById('2405.01631v1-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">16 pages, 10+A2 figures. Accepted for publication on Astronomische Nachrichten on 2nd May 2024</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.03722">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/2403.12219">arXiv:2403.12219</a> <span> [<a href="https://arxiv.org/pdf/2403.12219">pdf</a>, <a href="https://arxiv.org/format/2403.12219">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202449560">10.1051/0004-6361/202449560 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> High-precision astrometry with VVV -- II. A near-infrared extension of Gaia into the Galactic plane </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Griggio%2C+M">M. Griggio</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=Bedin%2C+L+R">L. R. Bedin</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+L+C">L. C. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</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="2403.12219v2-abstract-short" style="display: inline;"> Aims. We use near-infrared, ground-based data from the VISTA Variables in the Via Lactea (VVV) survey to indirectly extend the astrometry provided by the Gaia catalog to objects in heavily-extincted regions towards the Galactic bulge and plane that are beyond Gaia's reach. Methods. We make use of the state-of-the-art techniques developed for high-precision astrometry and photometry with the Hubble… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.12219v2-abstract-full').style.display = 'inline'; document.getElementById('2403.12219v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.12219v2-abstract-full" style="display: none;"> Aims. We use near-infrared, ground-based data from the VISTA Variables in the Via Lactea (VVV) survey to indirectly extend the astrometry provided by the Gaia catalog to objects in heavily-extincted regions towards the Galactic bulge and plane that are beyond Gaia's reach. Methods. We make use of the state-of-the-art techniques developed for high-precision astrometry and photometry with the Hubble Space Telescope to process the VVV data. We employ empirical, spatially-variable, effective point-spread functions and local transformations to mitigate the effects of systematic errors, like residual geometric distortion and image motion, and to improve measurements in crowded fields and for faint stars. We also anchor our astrometry to the absolute reference frame of the Gaia Data Release 3. Results. We measure between 20 and 60 times more sources than Gaia in the region surrounding the Galactic center, obtaining an single-exposure precision of about 12 mas and a proper-motion precision of better than 1 mas yr$^{-1}$ for bright, unsaturated sources. Our astrometry provides an extension of Gaia into the Galactic center. We publicly release the astro-photometric catalogs of the two VVV fields considered in this work, which contain a total of $\sim$ 3.5 million sources. Our catalogs cover $\sim$ 3 sq. degrees, about 0.5% of the entire VVV survey area. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.12219v2-abstract-full').style.display = 'none'; document.getElementById('2403.12219v2-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 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 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">10 pages, 13 figures, accepted for publication in A&A on March 18, 2024</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 687, A94 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.03262">arXiv:2403.03262</a> <span> [<a href="https://arxiv.org/pdf/2403.03262">pdf</a>, <a href="https://arxiv.org/format/2403.03262">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The $\textit{HST}$ Large Programme on NGC$\,$6752 -- V. Differences in Luminosity and Mass Functions among Multiple Stellar Populations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Scalco%2C+M">M. Scalco</a>, <a href="/search/astro-ph?searchtype=author&query=Gerasimov%2C+R">R. Gerasimov</a>, <a href="/search/astro-ph?searchtype=author&query=Bedin%2C+L+R">L. R. Bedin</a>, <a href="/search/astro-ph?searchtype=author&query=Vesperini%2C+E">E. Vesperini</a>, <a href="/search/astro-ph?searchtype=author&query=Nardiello%2C+D">D. Nardiello</a>, <a href="/search/astro-ph?searchtype=author&query=Salaris%2C+M">M. Salaris</a>, <a href="/search/astro-ph?searchtype=author&query=Burgasser%2C+A">A. Burgasser</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">J. Anderson</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=Rosati%2C+P">P. Rosati</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="2403.03262v1-abstract-short" style="display: inline;"> We exploit the astro-photometric dataset of the multi-epoch infrared parallel field of a $\textit{Hubble Space Telescope}$ Large Programme aimed at studying the faintest stars of the globular cluster NGC$\,$6752 to determine the luminosity and mass functions of the multiple stellar populations of this cluster. Thanks to the measurement of proper motions and deeper completeness, the results present… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.03262v1-abstract-full').style.display = 'inline'; document.getElementById('2403.03262v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.03262v1-abstract-full" style="display: none;"> We exploit the astro-photometric dataset of the multi-epoch infrared parallel field of a $\textit{Hubble Space Telescope}$ Large Programme aimed at studying the faintest stars of the globular cluster NGC$\,$6752 to determine the luminosity and mass functions of the multiple stellar populations of this cluster. Thanks to the measurement of proper motions and deeper completeness, the results presented in this paper represent a significant improvement over those of previous studies. We successfully derived membership probabilities reaching stars as faint as $m_{\rm F160W} \sim 25$, allowing us to reliably distinguish the three main stellar populations detected within this cluster. We employed a new set of model isochrones that have been individually fit to the colour-magnitude diagram of each population. We present a comprehensive analysis of the luminosity and mass functions for three stellar populations within NGC$\,$6752. Notably, our findings reveal differences in the present-day luminosity and mass functions of first-generation and second-generation stars; these differences are consistent with the manifestation of the effects of dynamical processes acting on populations with different initial spatial distributions. Finally, we publicly release the catalogues with positions, photometry, proper motions, and memberships probabilities, as well as the stacked-image atlases and all newly calculated stellar models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.03262v1-abstract-full').style.display = 'none'; document.getElementById('2403.03262v1-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 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">25 pages, 17 figures, 5 tables. Accepted for publication in AN</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.09902">arXiv:2310.09902</a> <span> [<a href="https://arxiv.org/pdf/2310.09902">pdf</a>, <a href="https://arxiv.org/format/2310.09902">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> </div> </div> <p class="title is-5 mathjax"> JWST-TST High Contrast: Achieving direct spectroscopy of faint substellar companions next to bright stars with the NIRSpec IFU </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ruffio%2C+J">Jean-Baptiste Ruffio</a>, <a href="/search/astro-ph?searchtype=author&query=Perrin%2C+M+D">Marshall D. Perrin</a>, <a href="/search/astro-ph?searchtype=author&query=Hoch%2C+K+K+W">Kielan K. W. Hoch</a>, <a href="/search/astro-ph?searchtype=author&query=Kammerer%2C+J">Jens Kammerer</a>, <a href="/search/astro-ph?searchtype=author&query=Konopacky%2C+Q+M">Quinn M. Konopacky</a>, <a href="/search/astro-ph?searchtype=author&query=Pueyo%2C+L">Laurent Pueyo</a>, <a href="/search/astro-ph?searchtype=author&query=Madurowicz%2C+A">Alex Madurowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Rickman%2C+E">Emily Rickman</a>, <a href="/search/astro-ph?searchtype=author&query=Theissen%2C+C+A">Christopher A. Theissen</a>, <a href="/search/astro-ph?searchtype=author&query=Agrawal%2C+S">Shubh Agrawal</a>, <a href="/search/astro-ph?searchtype=author&query=Greenbaum%2C+A+Z">Alexandra Z. Greenbaum</a>, <a href="/search/astro-ph?searchtype=author&query=Miles%2C+B+E">Brittany E. Miles</a>, <a href="/search/astro-ph?searchtype=author&query=Barman%2C+T+S">Travis S. Barman</a>, <a href="/search/astro-ph?searchtype=author&query=Balmer%2C+W+O">William O. Balmer</a>, <a href="/search/astro-ph?searchtype=author&query=Llop-Sayson%2C+J">Jorge Llop-Sayson</a>, <a href="/search/astro-ph?searchtype=author&query=Girard%2C+J+H">Julien H. Girard</a>, <a href="/search/astro-ph?searchtype=author&query=Rebollido%2C+I">Isabel Rebollido</a>, <a href="/search/astro-ph?searchtype=author&query=Soummer%2C+R">R茅mi Soummer</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+N+H">Natalie H. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">Jay Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Beichman%2C+C+A">Charles A. Beichman</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">Andrea Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Bryden%2C+G">Geoffrey Bryden</a>, <a href="/search/astro-ph?searchtype=author&query=Espinoza%2C+N">N茅stor Espinoza</a>, <a href="/search/astro-ph?searchtype=author&query=Glidden%2C+A">Ana Glidden</a> , et al. (11 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.09902v2-abstract-short" style="display: inline;"> The JWST NIRSpec integral field unit (IFU) presents a unique opportunity to observe directly imaged exoplanets from 3-5 um at moderate spectral resolution (R~2,700) and thereby better constrain the composition, disequilibrium chemistry, and cloud properties of their atmospheres. In this work, we present the first NIRSpec IFU high-contrast observations of a substellar companion that requires starli… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.09902v2-abstract-full').style.display = 'inline'; document.getElementById('2310.09902v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.09902v2-abstract-full" style="display: none;"> The JWST NIRSpec integral field unit (IFU) presents a unique opportunity to observe directly imaged exoplanets from 3-5 um at moderate spectral resolution (R~2,700) and thereby better constrain the composition, disequilibrium chemistry, and cloud properties of their atmospheres. In this work, we present the first NIRSpec IFU high-contrast observations of a substellar companion that requires starlight suppression techniques. We develop specific data reduction strategies to study faint companions around bright stars, and assess the performance of NIRSpec at high contrast. First, we demonstrate an approach to forward model the companion signal and the starlight directly in the detector images, which mitigates the effects of NIRSpec's spatial undersampling. We demonstrate a sensitivity to planets that are 3e-6 fainter than their stars at 1'', or 3e-5 at 0.3''. Then, we implement a reference star point spread function (PSF) subtraction and a spectral extraction that does not require spatially and spectrally regularly sampled spectral cubes. This allows us to extract a moderate resolution (R~2,700) spectrum of the faint T-dwarf companion HD 19467 B from 2.9-5.2 um with signal-to-noise ratio (S/N)~10 per resolution element. Across this wavelength range, HD~19467~B has a flux ratio varying between 1e-5-1e-4 and a separation relative to its star of 1.6''. A companion paper by Hoch et al. more deeply analyzes the atmospheric properties of this companion based on the extracted spectrum. Using the methods developed here, NIRSpec's sensitivity may enable direct detection and spectral characterization of relatively old (~1 Gyr), cool (~250 K), and closely separated (~3-5 au) exoplanets that are less massive than Jupiter. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.09902v2-abstract-full').style.display = 'none'; document.getElementById('2310.09902v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to AJ. The data analysis scripts for this work are published https://github.com/jruffio/HD_19467_B (https://zenodo.org/doi/10.5281/zenodo.11391740). The main revisions of the manuscript are listed in the change history section of the readme</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.08637">arXiv:2310.08637</a> <span> [<a href="https://arxiv.org/pdf/2310.08637">pdf</a>, <a href="https://arxiv.org/format/2310.08637">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> <p class="title is-5 mathjax"> JWST-TST DREAMS: Quartz Clouds in the Atmosphere of WASP-17b </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Grant%2C+D">David Grant</a>, <a href="/search/astro-ph?searchtype=author&query=Lewis%2C+N+K">Nikole K. Lewis</a>, <a href="/search/astro-ph?searchtype=author&query=Wakeford%2C+H+R">Hannah R. Wakeford</a>, <a href="/search/astro-ph?searchtype=author&query=Batalha%2C+N+E">Natasha E. Batalha</a>, <a href="/search/astro-ph?searchtype=author&query=Glidden%2C+A">Ana Glidden</a>, <a href="/search/astro-ph?searchtype=author&query=Goyal%2C+J">Jayesh Goyal</a>, <a href="/search/astro-ph?searchtype=author&query=Mullens%2C+E">Elijah Mullens</a>, <a href="/search/astro-ph?searchtype=author&query=MacDonald%2C+R+J">Ryan J. MacDonald</a>, <a href="/search/astro-ph?searchtype=author&query=May%2C+E+M">Erin M. May</a>, <a href="/search/astro-ph?searchtype=author&query=Seager%2C+S">Sara Seager</a>, <a href="/search/astro-ph?searchtype=author&query=Stevenson%2C+K+B">Kevin B. Stevenson</a>, <a href="/search/astro-ph?searchtype=author&query=Valenti%2C+J+A">Jeff A. Valenti</a>, <a href="/search/astro-ph?searchtype=author&query=Visscher%2C+C">Channon Visscher</a>, <a href="/search/astro-ph?searchtype=author&query=Alderson%2C+L">Lili Alderson</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+N+H">Natalie H. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Ca%C3%B1as%2C+C+I">Caleb I. Ca帽as</a>, <a href="/search/astro-ph?searchtype=author&query=Col%C3%B3n%2C+K">Knicole Col贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Clampin%2C+M">Mark Clampin</a>, <a href="/search/astro-ph?searchtype=author&query=Espinoza%2C+N">N茅stor Espinoza</a>, <a href="/search/astro-ph?searchtype=author&query=Gressier%2C+A">Am茅lie Gressier</a>, <a href="/search/astro-ph?searchtype=author&query=Huang%2C+J">Jingcheng Huang</a>, <a href="/search/astro-ph?searchtype=author&query=Lin%2C+Z">Zifan Lin</a>, <a href="/search/astro-ph?searchtype=author&query=Long%2C+D">Douglas Long</a>, <a href="/search/astro-ph?searchtype=author&query=Louie%2C+D+R">Dana R. Louie</a>, <a href="/search/astro-ph?searchtype=author&query=Pe%C3%B1a-Guerrero%2C+M">Maria Pe帽a-Guerrero</a> , et al. (17 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.08637v2-abstract-short" style="display: inline;"> Clouds are prevalent in many of the exoplanet atmospheres that have been observed to date. For transiting exoplanets, we know if clouds are present because they mute spectral features and cause wavelength-dependent scattering. While the exact composition of these clouds is largely unknown, this information is vital to understanding the chemistry and energy budget of planetary atmospheres. In this… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.08637v2-abstract-full').style.display = 'inline'; document.getElementById('2310.08637v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.08637v2-abstract-full" style="display: none;"> Clouds are prevalent in many of the exoplanet atmospheres that have been observed to date. For transiting exoplanets, we know if clouds are present because they mute spectral features and cause wavelength-dependent scattering. While the exact composition of these clouds is largely unknown, this information is vital to understanding the chemistry and energy budget of planetary atmospheres. In this work, we observe one transit of the hot Jupiter WASP-17b with JWST's MIRI LRS and generate a transmission spectrum from 5-12 $\rm渭$m. These wavelengths allow us to probe absorption due to the vibrational modes of various predicted cloud species. Our transmission spectrum shows additional opacity centered at 8.6 $\rm渭$m, and detailed atmospheric modeling and retrievals identify this feature as SiO$_2$(s) (quartz) clouds. The SiO$_2$(s) clouds model is preferred at 3.5-4.2$蟽$ versus a cloud-free model and at 2.6$蟽$ versus a generic aerosol prescription. We find the SiO$_2$(s) clouds are comprised of small ${\sim}0.01$ $\rm渭$m particles, which extend to high altitudes in the atmosphere. The atmosphere also shows a depletion of H$_2$O, a finding consistent with the formation of high-temperature aerosols from oxygen-rich species. This work is part of a series of studies by our JWST Telescope Scientist Team (JWST-TST), in which we will use Guaranteed Time Observations to perform Deep Reconnaissance of Exoplanet Atmospheres through Multi-instrument Spectroscopy (DREAMS). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.08637v2-abstract-full').style.display = 'none'; document.getElementById('2310.08637v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 7 figures, fixed typo in Equation 3</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.02503">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/2306.10647">arXiv:2306.10647</a> <span> [<a href="https://arxiv.org/pdf/2306.10647">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Roman CCS White Paper: Adding Fields Hosting Globular Clusters To The Galactic Bulge Time Domain Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Grunblatt%2C+S+K">Samuel K. Grunblatt</a>, <a href="/search/astro-ph?searchtype=author&query=Wilson%2C+R+F">Robert F. Wilson</a>, <a href="/search/astro-ph?searchtype=author&query=Winter%2C+A">Andrew Winter</a>, <a href="/search/astro-ph?searchtype=author&query=Gaudi%2C+B+S">B. Scott Gaudi</a>, <a href="/search/astro-ph?searchtype=author&query=Huber%2C+D">Daniel Huber</a>, <a href="/search/astro-ph?searchtype=author&query=Yahalomi%2C+D+A">Daniel A. Yahalomi</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">Andrea Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Claytor%2C+Z+R">Zachary R. Claytor</a>, <a href="/search/astro-ph?searchtype=author&query=Palomera%2C+J+M">Jorge Martinez Palomera</a>, <a href="/search/astro-ph?searchtype=author&query=Barclay%2C+T">Thomas Barclay</a>, <a href="/search/astro-ph?searchtype=author&query=Fu%2C+G">Guangwei Fu</a>, <a href="/search/astro-ph?searchtype=author&query=Price-Whelan%2C+A">Adrian Price-Whelan</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="2306.10647v1-abstract-short" style="display: inline;"> Despite multiple previous searches, no transiting planets have yet been identified within a globular cluster. This is believed to be due to a combination of factors: the low metallicities of most globular clusters suggests that there is significantly less planet-forming material per star in most globular clusters relative to the solar neighborhood, the high likelihood of dynamical interactions can… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.10647v1-abstract-full').style.display = 'inline'; document.getElementById('2306.10647v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.10647v1-abstract-full" style="display: none;"> Despite multiple previous searches, no transiting planets have yet been identified within a globular cluster. This is believed to be due to a combination of factors: the low metallicities of most globular clusters suggests that there is significantly less planet-forming material per star in most globular clusters relative to the solar neighborhood, the high likelihood of dynamical interactions can also disrupt planetary orbits, and the data available for globular clusters is limited. However, transiting planets have been identified in open clusters, indicating that there may be planets in more massive clusters that have simply gone undetected, or that more massive clusters inhibit planet formation. Less than two degrees away from the nominal Galactic Bulge Time Domain Survey footprint, two globular clusters, NGC 6522 and NGC 6528, can be simultaneously observed by the Roman telescope during the Galactic Bulge Time Domain Survey. These clusters are comparable in mass (1-2 x 10$^5$ solar masses) and age (12 Gyr), but feature drastically different average metallicities: NGC 6522 has an average [Fe/H] $\sim$ -1.3, while NGC 6528 has an average [Fe/H] $\sim$ -0.1. If no transiting planets are detected in one season of time domain observations of these clusters, this would indicate a difference in planet occurrence among field stars and globular clusters at >3-$蟽$ significance even after accounting for metallicity, which could be enhanced to >5-$蟽$ significance with similar observations of another nearby field hosting a metal-rich globular cluster. Additionally, time domain observations of NGC 6522 and NGC 6528 will detect variable stars in both clusters, testing the connection between stellar variability and binary fraction to metallicity and cluster environment, as well as testing the dependence of exoplanet yields on stellar density and distance from the Galactic midplane. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.10647v1-abstract-full').style.display = 'none'; document.getElementById('2306.10647v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages, 3 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/2305.12702">arXiv:2305.12702</a> <span> [<a href="https://arxiv.org/pdf/2305.12702">pdf</a>, <a href="https://arxiv.org/format/2305.12702">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="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stad1068">10.1093/mnras/stad1068 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An elusive dark central mass in the globular cluster M4 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vitral%2C+E">Eduardo Vitral</a>, <a href="/search/astro-ph?searchtype=author&query=Libralato%2C+M">Mattia Libralato</a>, <a href="/search/astro-ph?searchtype=author&query=Kremer%2C+K">Kyle Kremer</a>, <a href="/search/astro-ph?searchtype=author&query=Mamon%2C+G+A">Gary A. Mamon</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">Andrea Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Bedin%2C+L+R">Luigi R. Bedin</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">Jay Anderson</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="2305.12702v1-abstract-short" style="display: inline;"> Recent studies of nearby globular clusters have discovered excess dark mass in their cores, apparently in an extended distribution, and simulations indicate that this mass is composed mostly of white dwarfs (respectively stellar-mass black holes) in clusters that are core-collapsed (respectively with a flatter core). We perform mass-anisotropy modelling of the closest globular cluster, M4, with in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.12702v1-abstract-full').style.display = 'inline'; document.getElementById('2305.12702v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.12702v1-abstract-full" style="display: none;"> Recent studies of nearby globular clusters have discovered excess dark mass in their cores, apparently in an extended distribution, and simulations indicate that this mass is composed mostly of white dwarfs (respectively stellar-mass black holes) in clusters that are core-collapsed (respectively with a flatter core). We perform mass-anisotropy modelling of the closest globular cluster, M4, with intermediate slope for the inner stellar density. We use proper-motion data from Gaia EDR3 and from observations by the Hubble Space Telescope. We extract the mass profile employing Bayesian Jeans modelling, and check our fits with realistic mock data. Our analyses return isotropic motions in the cluster core and tangential motions ($尾\approx -0.4$$\pm$$0.1$) in the outskirts. We also robustly measure a dark central mass of roughly $800\pm300 \,$M$_{\odot}$, but it is not possible to distinguish between a point-like source, such as an intermediate-mass black hole (IMBH), or a dark population of stellar remnants of extent $\approx 0.016\,\rm pc \simeq 3300\,AU$. However, when removing a high-velocity star from the cluster centre, the same mass excess is found, but more extended ($\sim 0.034\, \rm{pc} \approx 7000\,\rm AU$). We use Monte Carlo $N$-body models of M4 to interpret the second outcome, and find that our excess mass is not sufficiently extended to be confidently associated with a dark population of remnants. Finally, we discuss the feasibility of these two scenarios (i.e., IMBH vs. remnants), and propose new observations that could help to better grasp the complex dynamics in M4's core. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.12702v1-abstract-full').style.display = 'none'; document.getElementById('2305.12702v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 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">19 page, 15 figures, 3 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/2303.15253">arXiv:2303.15253</a> <span> [<a href="https://arxiv.org/pdf/2303.15253">pdf</a>, <a href="https://arxiv.org/format/2303.15253">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/mnrasl/slad042">10.1093/mnrasl/slad042 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First observational evidence of a relation between globular clusters' internal rotation and stellar masses </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Scalco%2C+M">M. Scalco</a>, <a href="/search/astro-ph?searchtype=author&query=Livernois%2C+A">A. Livernois</a>, <a href="/search/astro-ph?searchtype=author&query=Vesperini%2C+E">E. Vesperini</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=Bedin%2C+L+R">L. R. Bedin</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.15253v1-abstract-short" style="display: inline;"> Several observational studies have shown that many Galactic globular clusters (GCs) are characterised by internal rotation. Theoretical studies of the dynamical evolution of rotating clusters have predicted that, during their long-term evolution, these stellar systems should develop a dependence of the rotational velocity around the cluster's centre on the mass of stars, with the internal rotation… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.15253v1-abstract-full').style.display = 'inline'; document.getElementById('2303.15253v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.15253v1-abstract-full" style="display: none;"> Several observational studies have shown that many Galactic globular clusters (GCs) are characterised by internal rotation. Theoretical studies of the dynamical evolution of rotating clusters have predicted that, during their long-term evolution, these stellar systems should develop a dependence of the rotational velocity around the cluster's centre on the mass of stars, with the internal rotation increasing for more massive stars. In this paper we present the first observational evidence of the predicted rotation-mass trend. In our investigation, we exploited the $\mathit{Gaia}$ Data Release 3 catalogue of three GCs: NGC 104 (47 Tuc), NGC 5139 ($蠅$ Cen) and NGC 5904 (M 5). We found clear evidence of a cluster rotation-mass relation in 47 Tuc and M 5, while in $蠅$ Cen, the dynamically youngest system among the three clusters studied here, no such trend was detected. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.15253v1-abstract-full').style.display = 'none'; document.getElementById('2303.15253v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">6 pages, 4 figures, 1 table. Accepted for publication in MNRAS Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.00009">arXiv:2303.00009</a> <span> [<a href="https://arxiv.org/pdf/2303.00009">pdf</a>, <a href="https://arxiv.org/format/2303.00009">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/acd04f">10.3847/1538-4357/acd04f <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> JWST-TST Proper Motions: I. High-Precision NIRISS Calibration and Large Magellanic Cloud Kinematics </p> <p class="authors"> <span class="search-hit">Authors:</span> <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+der+Marel%2C+R+P">R. P. van der Marel</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Sohn%2C+S+T">S. T. Sohn</a>, <a href="/search/astro-ph?searchtype=author&query=Watkins%2C+L+L">L. L. Watkins</a>, <a href="/search/astro-ph?searchtype=author&query=Alderson%2C+L">L. Alderson</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+N">N. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Clampin%2C+M">M. Clampin</a>, <a href="/search/astro-ph?searchtype=author&query=Glidden%2C+A">A. Glidden</a>, <a href="/search/astro-ph?searchtype=author&query=Goyal%2C+J">J. Goyal</a>, <a href="/search/astro-ph?searchtype=author&query=Hoch%2C+K">K. Hoch</a>, <a href="/search/astro-ph?searchtype=author&query=Huang%2C+J">J. Huang</a>, <a href="/search/astro-ph?searchtype=author&query=Kammerer%2C+J">J. Kammerer</a>, <a href="/search/astro-ph?searchtype=author&query=Lewis%2C+N+K">N. K. Lewis</a>, <a href="/search/astro-ph?searchtype=author&query=Lin%2C+Z">Z. Lin</a>, <a href="/search/astro-ph?searchtype=author&query=Long%2C+D">D. Long</a>, <a href="/search/astro-ph?searchtype=author&query=Louie%2C+D">D. Louie</a>, <a href="/search/astro-ph?searchtype=author&query=MacDonald%2C+R+J">R. J. MacDonald</a>, <a href="/search/astro-ph?searchtype=author&query=Mountain%2C+M">M. Mountain</a>, <a href="/search/astro-ph?searchtype=author&query=Pe%C3%B1a-Guerrero%2C+M">M. Pe帽a-Guerrero</a>, <a href="/search/astro-ph?searchtype=author&query=Perrin%2C+M+D">M. D. Perrin</a>, <a href="/search/astro-ph?searchtype=author&query=Pueyo%2C+L">L. Pueyo</a>, <a href="/search/astro-ph?searchtype=author&query=Rebollido%2C+I">I. Rebollido</a>, <a href="/search/astro-ph?searchtype=author&query=Rickman%2C+E">E. Rickman</a> , et al. (5 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.00009v2-abstract-short" style="display: inline;"> We develop and disseminate effective point-spread functions and geometric-distortion solutions for high-precision astrometry and photometry with the JWST NIRISS instrument. We correct field dependencies and detector effects, and assess the quality and the temporal stability of the calibrations. As a scientific application and validation, we study the proper motion (PM) kinematics of stars in the J… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.00009v2-abstract-full').style.display = 'inline'; document.getElementById('2303.00009v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.00009v2-abstract-full" style="display: none;"> We develop and disseminate effective point-spread functions and geometric-distortion solutions for high-precision astrometry and photometry with the JWST NIRISS instrument. We correct field dependencies and detector effects, and assess the quality and the temporal stability of the calibrations. As a scientific application and validation, we study the proper motion (PM) kinematics of stars in the JWST calibration field near the Large Magellanic Cloud (LMC) center, comparing to a first-epoch Hubble Space Telescope (HST) archival catalog with a 16-yr baseline. For stars with G~20, the median PM uncertainty is ~13 $渭$as yr$^{-1}$ (3.1 km s$^{-1}$), better than Gaia DR3 typically achieves for its very best-measured stars. We kinematically detect the known star cluster OGLE-CL LMC 407, measure its absolute PM for the first time, and show how this differs from other LMC populations. The inferred cluster dispersion sets an upper limit of 24 $渭$as yr$^{-1}$ (5.6 km s$^{-1}$) on systematic uncertainties. Red-giant-branch stars have a velocity dispersion of 33.8 $\pm$ 0.6 km s$^{-1}$, while younger blue populations have a narrower velocity distribution, but with a significant kinematical substructure. We discuss how this relates to the larger velocity dispersions inferred from Gaia DR3. These results establish JWST as capable of state-of-the-art astrometry, building on the extensive legacy of HST. This is the first paper in a series by our JWST Telescope Scientist Team (TST), in which we will use Guaranteed Time Observations to study the PM kinematics of various stellar systems in the Local Group. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.00009v2-abstract-full').style.display = 'none'; document.getElementById('2303.00009v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages, 25 figures, 2 tables. Accepted for publication in ApJ. The effective point-spread-function models, the geometric-distortion solutions and a preliminary version of the code are available at the links provided in the manuscript</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.04148">arXiv:2301.04148</a> <span> [<a href="https://arxiv.org/pdf/2301.04148">pdf</a>, <a href="https://arxiv.org/format/2301.04148">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/acaec6">10.3847/1538-4357/acaec6 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Hubble Space Telescope UV Legacy Survey of Galactic Globular Clusters. XXIV. Differences in internal kinematics of multiple stellar populations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Libralato%2C+M">M. Libralato</a>, <a href="/search/astro-ph?searchtype=author&query=Vesperini%2C+E">E. Vesperini</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">A. Bellini</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=van+der+Marel%2C+R+P">R. P. van der Marel</a>, <a href="/search/astro-ph?searchtype=author&query=Piotto%2C+G">G. Piotto</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Aparicio%2C+A">A. Aparicio</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">B. Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=Bedin%2C+L+R">L. R. Bedin</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+T+M">T. M. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Cassisi%2C+S">S. Cassisi</a>, <a href="/search/astro-ph?searchtype=author&query=Nardiello%2C+D">D. Nardiello</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">A. Sarajedini</a>, <a href="/search/astro-ph?searchtype=author&query=Scalco%2C+M">M. Scalco</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="2301.04148v2-abstract-short" style="display: inline;"> Our understanding of the kinematic properties of multiple stellar populations (mPOPs) in Galactic globular clusters (GCs) is still limited compared to what we know about their chemical and photometric characteristics. Such limitation arises from the lack of a comprehensive observational investigation of this topic. Here we present the first homogeneous kinematic analysis of mPOPs in 56 GCs based o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.04148v2-abstract-full').style.display = 'inline'; document.getElementById('2301.04148v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.04148v2-abstract-full" style="display: none;"> Our understanding of the kinematic properties of multiple stellar populations (mPOPs) in Galactic globular clusters (GCs) is still limited compared to what we know about their chemical and photometric characteristics. Such limitation arises from the lack of a comprehensive observational investigation of this topic. Here we present the first homogeneous kinematic analysis of mPOPs in 56 GCs based on high-precision proper motions computed with Hubble Space Telescope data. We focused on red-giant-branch stars, for which the mPOP tagging is clearer, and measured the velocity dispersion of stars belonging to first (1G) and second generations (2G). We find that 1G stars are generally kinematically isotropic even at the half-light radius, whereas 2G stars are isotropic at the center and become radially anisotropic before the half-light radius. The radial anisotropy is induced by a lower tangential velocity dispersion of 2G stars with respect to the 1G population, while the radial component of the motion is comparable. We also show possible evidence that the kinematic properties of mPOPs are affected by the Galactic tidal field, corroborating previous observational and theoretical results suggesting a relation between the strength of the external tidal field and some properties of mPOPs. Although limited to the GCs' central regions, our analysis leads to new insights into the mPOP phenomenon, and provides the motivation for future observational studies of the internal kinematics of mPOPs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.04148v2-abstract-full').style.display = 'none'; document.getElementById('2301.04148v2-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 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 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">10 pages, 4 figures, 2 tables. Accepted for publication on 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/2212.07978">arXiv:2212.07978</a> <span> [<a href="https://arxiv.org/pdf/2212.07978">pdf</a>, <a href="https://arxiv.org/format/2212.07978">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202244798">10.1051/0004-6361/202244798 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Hubble Space Telescope survey of Magellanic Cloud star clusters. Photometry and astrometry of 113 clusters and early results </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Milone%2C+A+P">A. P. Milone</a>, <a href="/search/astro-ph?searchtype=author&query=Cordoni%2C+G">G. Cordoni</a>, <a href="/search/astro-ph?searchtype=author&query=Marino%2C+A+F">A. F. Marino</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Antona%2C+F">F. D'Antona</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">A. Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Criscienzo%2C+M">M. Di Criscienzo</a>, <a href="/search/astro-ph?searchtype=author&query=Dondoglio%2C+E">E. Dondoglio</a>, <a href="/search/astro-ph?searchtype=author&query=Lagioia%2C+E+P">E. P. Lagioia</a>, <a href="/search/astro-ph?searchtype=author&query=Langer%2C+N">N. Langer</a>, <a href="/search/astro-ph?searchtype=author&query=Legnardi%2C+M+V">M. V. Legnardi</a>, <a href="/search/astro-ph?searchtype=author&query=Libralato%2C+M">M. Libralato</a>, <a href="/search/astro-ph?searchtype=author&query=Baumgardt%2C+H">H. Baumgardt</a>, <a href="/search/astro-ph?searchtype=author&query=Bettinelli%2C+M">M. Bettinelli</a>, <a href="/search/astro-ph?searchtype=author&query=Cavecchi%2C+Y">Y. Cavecchi</a>, <a href="/search/astro-ph?searchtype=author&query=de+Grijs%2C+R">R. de Grijs</a>, <a href="/search/astro-ph?searchtype=author&query=Deng%2C+L">L. Deng</a>, <a href="/search/astro-ph?searchtype=author&query=Hastings%2C+B">B. Hastings</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+C">C. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Mohandasan%2C+A">A. Mohandasan</a>, <a href="/search/astro-ph?searchtype=author&query=Renzini%2C+A">A. Renzini</a>, <a href="/search/astro-ph?searchtype=author&query=Vesperini%2C+E">E. Vesperini</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+C">C. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Ziliotto%2C+T">T. Ziliotto</a>, <a href="/search/astro-ph?searchtype=author&query=Carlos%2C+M">M. Carlos</a>, <a href="/search/astro-ph?searchtype=author&query=Costa%2C+G">G. Costa</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="2212.07978v1-abstract-short" style="display: inline;"> In the past years, we have undertaken an extensive investigation of LMC and SMC star clusters based on HST data. We present photometry and astrometry of stars in 101 fields observed with the WFC/ACS, UVIS/WFC3 and NIR/WFC3 cameras. These fields comprise 113 star clusters. We provide differential-reddening maps and illustrate various scientific outcomes that arise from the early inspection of the p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.07978v1-abstract-full').style.display = 'inline'; document.getElementById('2212.07978v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.07978v1-abstract-full" style="display: none;"> In the past years, we have undertaken an extensive investigation of LMC and SMC star clusters based on HST data. We present photometry and astrometry of stars in 101 fields observed with the WFC/ACS, UVIS/WFC3 and NIR/WFC3 cameras. These fields comprise 113 star clusters. We provide differential-reddening maps and illustrate various scientific outcomes that arise from the early inspection of the photometric catalogs. In particular, we provide new insights on the extended main-sequence turn-off (eMSTO) phenomenon: i) We detected eMSTOs in two clusters, KMHK361 and NGC265, which had no previous evidence of multiple populations. This finding corroborates the conclusion that the eMSTO is a widespread phenomenon among clusters younger than ~2 Gyr. ii) The homogeneous color-magnitude diagrams (CMDs) of 19 LMC clusters reveal that the distribution of stars along the eMSTO depends on cluster age. iii) We discovered a new feature along the eMSTO of NGC1783, which consists of a distinct group of stars going on the red side of the eMSTO in CMDs composed of ultraviolet filters. Furthermore, we derived the proper motions of stars in the fields of view of clusters with multi-epoch images. Proper motions allowed us to separate the bulk of bright field stars from cluster members and investigate the internal kinematics of stellar populations in various LMC and SMC fields. As an example, we analyze the field around NGC346 to disentangle the motions of its stellar populations, including NGC364 and BS90, young and pre-MS stars in the star-forming region associated with NGC346, and young and old field stellar populations of the SMC. Based on these results and the fields around five additional clusters, we find that young SMC stars exhibit elongated proper-motion distributions that point toward the LMC, thus bringing new evidence for a kinematic connection between the LMC and SMC. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.07978v1-abstract-full').style.display = 'none'; document.getElementById('2212.07978v1-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 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">37 pages, 27 figures, accepted for publication in Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 672, A161 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.02391">arXiv:2211.02391</a> <span> [<a href="https://arxiv.org/pdf/2211.02391">pdf</a>, <a href="https://arxiv.org/format/2211.02391">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stac3219">10.1093/mnras/stac3219 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The HST large programme on NGC 6752 -- IV. The White Dwarf Sequence </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bedin%2C+L+R">L. R. Bedin</a>, <a href="/search/astro-ph?searchtype=author&query=Salaris%2C+M">M. Salaris</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Scalco%2C+M">M. Scalco</a>, <a href="/search/astro-ph?searchtype=author&query=Nardiello%2C+D">D. Nardiello</a>, <a href="/search/astro-ph?searchtype=author&query=Vesperini%2C+E">E. Vesperini</a>, <a href="/search/astro-ph?searchtype=author&query=Richer%2C+H">H. Richer</a>, <a href="/search/astro-ph?searchtype=author&query=Burgasser%2C+A">A. Burgasser</a>, <a href="/search/astro-ph?searchtype=author&query=Griggio%2C+M">M. Griggio</a>, <a href="/search/astro-ph?searchtype=author&query=Gerasimov%2C+R">R. Gerasimov</a>, <a href="/search/astro-ph?searchtype=author&query=Apai%2C+D">D. Apai</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=Bergeron%2C+P">P. Bergeron</a>, <a href="/search/astro-ph?searchtype=author&query=Rich%2C+R+M">R. M. Rich</a>, <a href="/search/astro-ph?searchtype=author&query=Grazian%2C+A">A. Grazian</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="2211.02391v1-abstract-short" style="display: inline;"> We present our final study of the white dwarf cooling sequence (WD CS) in the globular cluster NGC 6752. The investigation is the main goal of a dedicated Hubble Space Telescope large Program, for which all the observations are now collected. The WD CS luminosity function (LF) is confirmed to peak at m_F606W = 29.3+/-0.1, consistent within uncertainties with what has been previously reported, and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.02391v1-abstract-full').style.display = 'inline'; document.getElementById('2211.02391v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.02391v1-abstract-full" style="display: none;"> We present our final study of the white dwarf cooling sequence (WD CS) in the globular cluster NGC 6752. The investigation is the main goal of a dedicated Hubble Space Telescope large Program, for which all the observations are now collected. The WD CS luminosity function (LF) is confirmed to peak at m_F606W = 29.3+/-0.1, consistent within uncertainties with what has been previously reported, and is now complete down to m_F606W~29.7. We have performed robust and conclusive comparisons with model predictions that show how the theoretical LF for hydrogen envelope WD models closely follow the shape of the empirical LF. The magnitude of the peak of the observed LF is matched with ages between 12.7 and 13.5 Gyr, consistent with the cluster age derived from the main sequence turn off and subgiant branch. We also find that the impact of multiple populations within the cluster on the WD LF for m_F606W below 27.3 is negligible, and that the presence of a small fraction of helium envelope objects is consistent with the data. Our analysis reveals a possible hint of an underestimate of the cooling timescales of models in the magnitude range 28.1 < m_F606W < 28.9. Finally, we find that hydrogen envelope models calculated with a new tabulation of electron conduction opacities in the transition between moderate and strong degeneracy provide WD ages that are too small in comparison to the Main Sequence turnoff age. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.02391v1-abstract-full').style.display = 'none'; document.getElementById('2211.02391v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 13 figures. Accepted for publication in MNRAS on 2022, November 4. Associated files soon at this https://web.oapd.inaf.it/bedin/files/PAPERs_eMATERIALs/NGC6752_IV/</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.03179">arXiv:2207.03179</a> <span> [<a href="https://arxiv.org/pdf/2207.03179">pdf</a>, <a href="https://arxiv.org/format/2207.03179">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stac1920">10.1093/mnras/stac1920 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Astro-photometric study of M37 with Gaia and wide-field ugi-imaging </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Griggio%2C+M">M. Griggio</a>, <a href="/search/astro-ph?searchtype=author&query=Bedin%2C+L+R">L. R. Bedin</a>, <a href="/search/astro-ph?searchtype=author&query=Raddi%2C+R">R. Raddi</a>, <a href="/search/astro-ph?searchtype=author&query=Reindl%2C+N">N. Reindl</a>, <a href="/search/astro-ph?searchtype=author&query=Tomasella%2C+L">L. Tomasella</a>, <a href="/search/astro-ph?searchtype=author&query=Scalco%2C+M">M. Scalco</a>, <a href="/search/astro-ph?searchtype=author&query=Salaris%2C+M">M. Salaris</a>, <a href="/search/astro-ph?searchtype=author&query=Cassisi%2C+S">S. Cassisi</a>, <a href="/search/astro-ph?searchtype=author&query=Ochner%2C+P">P. Ochner</a>, <a href="/search/astro-ph?searchtype=author&query=Ciroi%2C+S">S. Ciroi</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Nardiello%2C+D">D. Nardiello</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">J. Anderson</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=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Spina%2C+L">L. Spina</a>, <a href="/search/astro-ph?searchtype=author&query=Pedani%2C+M">M. Pedani</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="2207.03179v1-abstract-short" style="display: inline;"> We present an astrometric and photometric wide-field study of the Galactic open star cluster M37 (NGC 2099). The studied field was observed with ground-based images covering a region of about four square degrees in the Sloan-like filters ugi. We exploited the Gaia catalogue to calibrate the geometric distortion of the large field mosaics, developing software routines that can be also applied to ot… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.03179v1-abstract-full').style.display = 'inline'; document.getElementById('2207.03179v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.03179v1-abstract-full" style="display: none;"> We present an astrometric and photometric wide-field study of the Galactic open star cluster M37 (NGC 2099). The studied field was observed with ground-based images covering a region of about four square degrees in the Sloan-like filters ugi. We exploited the Gaia catalogue to calibrate the geometric distortion of the large field mosaics, developing software routines that can be also applied to other wide-field instruments. The data are used to identify the hottest white dwarf (WD) member candidates of M37. Thanks to the Gaia EDR3 exquisite astrometry we identified seven such WD candidates, one of which, besides being a high-probability astrometric member, is the putative central star of a planetary nebula. To our knowledge, this is a unique object in an open cluster, and we have obtained follow-up low-resolution spectra that are used for a qualitative characterisation of this young WD. Finally, we publicly release a three-colour atlas and a catalogue of the sources in the field of view, which represents a complement of existing material. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.03179v1-abstract-full').style.display = 'none'; document.getElementById('2207.03179v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 July, 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">13 pages, 4 table, 13 figures. Accepted for publication in MNRAS on 2022, July 6, manuscript ID. MN-22-2264-MJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.09924">arXiv:2206.09924</a> <span> [<a href="https://arxiv.org/pdf/2206.09924">pdf</a>, <a href="https://arxiv.org/format/2206.09924">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/ac7727">10.3847/1538-4357/ac7727 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Hubble Space Telescope UV Legacy Survey of Galactic Globular Clusters. XXIII. Proper-motion catalogs and internal kinematics </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Vesperini%2C+E">E. Vesperini</a>, <a href="/search/astro-ph?searchtype=author&query=Piotto%2C+G">G. Piotto</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=van+der+Marel%2C+R+P">R. P. van der Marel</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Aparicio%2C+A">A. Aparicio</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">B. Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=Bedin%2C+L+R">L. R. Bedin</a>, <a href="/search/astro-ph?searchtype=author&query=Borsato%2C+L">L. Borsato</a>, <a href="/search/astro-ph?searchtype=author&query=Cassisi%2C+S">S. Cassisi</a>, <a href="/search/astro-ph?searchtype=author&query=Dalessandro%2C+E">E. Dalessandro</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraro%2C+F+R">F. R. Ferraro</a>, <a href="/search/astro-ph?searchtype=author&query=King%2C+I+R">I. R. King</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzoni%2C+B">B. Lanzoni</a>, <a href="/search/astro-ph?searchtype=author&query=Nardiello%2C+D">D. Nardiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ortolani%2C+S">S. Ortolani</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">A. Sarajedini</a>, <a href="/search/astro-ph?searchtype=author&query=Sohn%2C+S+T">S. T. Sohn</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2206.09924v2-abstract-short" style="display: inline;"> A number of studies based on data collected by the $\textit{Hubble Space Telescope}$ ($\textit{HST}$) GO-13297 program "HST Legacy Survey of Galactic Globular Clusters: Shedding UV Light on Their Populations and Formation" have investigated the photometric properties of a large sample of Galactic globular clusters and revolutionized our understanding of their stellar populations. In this paper, we… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.09924v2-abstract-full').style.display = 'inline'; document.getElementById('2206.09924v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.09924v2-abstract-full" style="display: none;"> A number of studies based on data collected by the $\textit{Hubble Space Telescope}$ ($\textit{HST}$) GO-13297 program "HST Legacy Survey of Galactic Globular Clusters: Shedding UV Light on Their Populations and Formation" have investigated the photometric properties of a large sample of Galactic globular clusters and revolutionized our understanding of their stellar populations. In this paper, we expand previous studies by focusing our attention on the stellar clusters' internal kinematics. We computed proper motions for stars in 56 globular and one open clusters by combining the GO-13297 images with archival $\textit{HST}$ data. The astro-photometric catalogs released with this paper represent the most complete and homogeneous collection of proper motions of stars in the cores of stellar clusters to date, and expand the information provided by the current (and future) $\textit{Gaia}$ data releases to much fainter stars and into the crowded central regions. We also census the general kinematic properties of stellar clusters by computing the velocity-dispersion and anisotropy radial profiles of their bright members. We study the dependence on concentration and relaxation time, and derive dynamical distances. Finally, we present an in-depth kinematic analysis of the globular cluster NGC 5904. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.09924v2-abstract-full').style.display = 'none'; document.getElementById('2206.09924v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">33 pages, 19 figures, 6 tables. Accepted for publication on ApJ. Astro-photometric catalogs, velocity-dispersion values and profiles are available at https://archive.stsci.edu/hlsp/hacks</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.05300">arXiv:2206.05300</a> <span> [<a href="https://arxiv.org/pdf/2206.05300">pdf</a>, <a href="https://arxiv.org/format/2206.05300">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/ac77f7">10.3847/1538-4357/ac77f7 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Hubble Space Telescope Proper Motion (HSTPROMO) Catalogs of Galactic Globular Clusters. VII. Energy Equipartition </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Watkins%2C+L+L">Laura L. Watkins</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=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=Anderson%2C+J">Jay Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro-Cuello%2C+M">Mayte 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="2206.05300v1-abstract-short" style="display: inline;"> We examine the degree of energy equipartition in 9 Galactic globular clusters using proper motions measured with the Hubble Space Telescope. For most clusters in the sample, this is the first energy equipartition study ever performed. This study is also the largest of its kind, albeit with only 9 clusters. We begin by rigorously cleaning the catalogues to remove poor-quality measurements and to en… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.05300v1-abstract-full').style.display = 'inline'; document.getElementById('2206.05300v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.05300v1-abstract-full" style="display: none;"> We examine the degree of energy equipartition in 9 Galactic globular clusters using proper motions measured with the Hubble Space Telescope. For most clusters in the sample, this is the first energy equipartition study ever performed. This study is also the largest of its kind, albeit with only 9 clusters. We begin by rigorously cleaning the catalogues to remove poor-quality measurements and to ensure high signal-to-noise for the study. Using the cleaned catalogues, we investigate how velocity dispersion $蟽$ changes with stellar mass $m$. We fit two functional forms: the first, a classic power-law of the form $蟽\propto m^{-畏}$ where $畏$ is the degree of energy equipartition, and the second from Bianchini et al. (2016) parameterised by an equipartition mass $m_{eq}$ where $畏$ changes with stellar mass. We find that both functions fit well but cannot distinguish with statistical significance which function provides the best fit. All clusters exhibit varying degrees of partial equipartition; no cluster is at or near full equipartition. We search for correlations of $畏$ and $m_{eq}$ with various cluster properties. The most significant correlation is observed with the number of core or median relaxation times ($N_{core}$ or $N_{half}$) the cluster has experienced. Finally, we determine the radial equipartition profile for each cluster, that is, how the degree of equipartition changes with projected distance from the cluster centre. We do not detect statistically significant trends in the degree of equipartition with radius. Overall, our observational findings are in broad agreement with theoretical predictions from N-body models published in recent years. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.05300v1-abstract-full').style.display = 'none'; document.getElementById('2206.05300v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">26 pages, 16 figures, 2 tables, accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.01814">arXiv:2206.01814</a> <span> [<a href="https://arxiv.org/pdf/2206.01814">pdf</a>, <a href="https://arxiv.org/format/2206.01814">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stac3532">10.1093/mnras/stac3532 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First semi-empirical test of the white dwarf mass-radius relationship using a single white dwarf via astrometric microlensing </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=McGill%2C+P">Peter McGill</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">Jay Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Casertano%2C+S">Stefano Casertano</a>, <a href="/search/astro-ph?searchtype=author&query=Sahu%2C+K+C">Kailash C. Sahu</a>, <a href="/search/astro-ph?searchtype=author&query=Bergeron%2C+P">Pierre Bergeron</a>, <a href="/search/astro-ph?searchtype=author&query=Blouin%2C+S">Simon Blouin</a>, <a href="/search/astro-ph?searchtype=author&query=Dufour%2C+P">Patrick Dufour</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+L+C">Leigh C. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+N+W">N. Wyn Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Belokurov%2C+V">Vasily Belokurov</a>, <a href="/search/astro-ph?searchtype=author&query=Smart%2C+R+L">Richard L. Smart</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">Andrea Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Calamida%2C+A">Annalisa Calamida</a>, <a href="/search/astro-ph?searchtype=author&query=Dominik%2C+M">Martin Dominik</a>, <a href="/search/astro-ph?searchtype=author&query=Kains%2C+N">No茅 Kains</a>, <a href="/search/astro-ph?searchtype=author&query=Kl%C3%BCter%2C+J">Jonas Kl眉ter</a>, <a href="/search/astro-ph?searchtype=author&query=Nielsen%2C+M+B">Martin Bo Nielsen</a>, <a href="/search/astro-ph?searchtype=author&query=Wambsganss%2C+J">Joachim Wambsganss</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2206.01814v2-abstract-short" style="display: inline;"> In November 2019, the nearby single, isolated DQ-type white dwarf LAWD 37 (WD 1142-645) aligned closely with a distant background source and caused an astrometric microlensing event. Leveraging astrometry from \Gaia{} and followup data from the \textit{Hubble Space Telescope} we measure the astrometric deflection of the background source and obtain a gravitational mass for LAWD~37. The main challe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.01814v2-abstract-full').style.display = 'inline'; document.getElementById('2206.01814v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.01814v2-abstract-full" style="display: none;"> In November 2019, the nearby single, isolated DQ-type white dwarf LAWD 37 (WD 1142-645) aligned closely with a distant background source and caused an astrometric microlensing event. Leveraging astrometry from \Gaia{} and followup data from the \textit{Hubble Space Telescope} we measure the astrometric deflection of the background source and obtain a gravitational mass for LAWD~37. The main challenge of this analysis is in extracting the lensing signal of the faint background source whilst it is buried in the wings of LAWD~37's point spread function. Removal of LAWD 37's point spread function induces a significant amount of correlated noise which we find can mimic the astrometric lensing signal. We find a deflection model including correlated noise caused by the removal of LAWD~37's point spread function best explains the data and yields a mass for LAWD 37 of $0.56\pm0.08 M_{\odot}$. This mass is in agreement with the theoretical mass-radius relationship and cooling tracks expected for CO core white dwarfs. Furthermore, the mass is consistent with no or trace amounts of hydrogen that is expected for objects with helium-rich atmospheres like LAWD 37. We conclude that further astrometric followup data on the source is likely to improve the inference on LAWD 37's mass at the $\approx3$ percent level and definitively rule out purely correlated noise explanations of the data. This work provides the first semi-empirical test of the white dwarf mass-radius relationship using a single, isolated white dwarf and supports current model atmospheres of DQ white dwarfs and white dwarf evolutionary theory. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.01814v2-abstract-full').style.display = 'none'; document.getElementById('2206.01814v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 pages, 18 figures, accepted to 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/2205.08009">arXiv:2205.08009</a> <span> [<a href="https://arxiv.org/pdf/2205.08009">pdf</a>, <a href="https://arxiv.org/format/2205.08009">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac70cf">10.3847/1538-4357/ac70cf <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> GaiaHub: A method for combining data from the Gaia and Hubble space telescopes to derive improved proper motions for faint stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=del+Pino%2C+A">Andr茅s del Pino</a>, <a href="/search/astro-ph?searchtype=author&query=Libralato%2C+M">Mattia Libralato</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=Bennet%2C+P">Paul Bennet</a>, <a href="/search/astro-ph?searchtype=author&query=Fardal%2C+M+A">Mark A. Fardal</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">Jay Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">Andrea Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Sohn%2C+S+T">Sangmo Tony Sohn</a>, <a href="/search/astro-ph?searchtype=author&query=Watkins%2C+L+L">Laura L. Watkins</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="2205.08009v1-abstract-short" style="display: inline;"> We present GaiaHub, a publicly available tool that combines $Gaia$ measurements with $Hubble$ $Space$ $Telescope$ ($HST$) archival images to derive proper motions (PMs). It increases the scientific impact of both observatories beyond their individual capabilities. $Gaia$ provides PMs across the whole sky, but the limited mirror size and time baseline restrict the best PM performance to relatively… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.08009v1-abstract-full').style.display = 'inline'; document.getElementById('2205.08009v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.08009v1-abstract-full" style="display: none;"> We present GaiaHub, a publicly available tool that combines $Gaia$ measurements with $Hubble$ $Space$ $Telescope$ ($HST$) archival images to derive proper motions (PMs). It increases the scientific impact of both observatories beyond their individual capabilities. $Gaia$ provides PMs across the whole sky, but the limited mirror size and time baseline restrict the best PM performance to relatively bright stars. $HST$ can measure accurate PMs for much fainter stars over a small field, but this requires two epochs of observation which are not always available. GaiaHub yields considerably improved PM accuracy compared to $Gaia$-only measurements, especially for faint sources $(G \gtrsim 18)$, requiring only a single epoch of $HST$ data observed more than $\sim 7$ years ago (before 2012). This provides considerable scientific value especially for dynamical studies of stellar systems or structures in and beyond the Milky Way (MW) halo, for which the member stars are generally faint. To illustrate the capabilities and demonstrate the accuracy of GaiaHub, we apply it to samples of MW globular clusters (GCs) and classical dwarf spheroidal (dSph) satellite galaxies. This allows us, e.g., to measure the velocity dispersions in the plane of the sky for objects out to and beyond $\sim 100$ kpc. We find, on average, mild radial velocity anisotropy in GCs, consistent with existing results for more nearby samples. We observe a correlation between the internal kinematics of the clusters and their ellipticity, with more isotropic clusters being, on average, more round. Our results also support previous findings that Draco and Sculptor dSph galaxies appear to be radially anisotropic systems. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.08009v1-abstract-full').style.display = 'none'; document.getElementById('2205.08009v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 18 figures. Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2202.07677">arXiv:2202.07677</a> <span> [<a href="https://arxiv.org/pdf/2202.07677">pdf</a>, <a href="https://arxiv.org/ps/2202.07677">ps</a>, <a href="https://arxiv.org/format/2202.07677">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/ac5406">10.3847/1538-4357/ac5406 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Blue Stragglers as tracers of the dynamical state of two clusters in the Small Magellanic Cloud: NGC 339 and NGC 419 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dresbach%2C+F">Francesca Dresbach</a>, <a href="/search/astro-ph?searchtype=author&query=Massari%2C+D">Davide Massari</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzoni%2C+B">Barbara Lanzoni</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraro%2C+F+R">Francesco R. Ferraro</a>, <a href="/search/astro-ph?searchtype=author&query=Dalessandro%2C+E">Emanuele Dalessandro</a>, <a href="/search/astro-ph?searchtype=author&query=Raso%2C+S">Silvia Raso</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> </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="2202.07677v1-abstract-short" style="display: inline;"> The level of central segregation of Blue Straggler stars proved to be an excellent tracer of the dynamical evolution of old star clusters (the so-called "dynamical clock"), both in the Milky Way and in the Large Magellanic Cloud. The $A^{+}$ parameter, used to measure the Blue Stragglers degree of segregation, has in fact been found to strongly correlate with the parent cluster central relaxation… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.07677v1-abstract-full').style.display = 'inline'; document.getElementById('2202.07677v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.07677v1-abstract-full" style="display: none;"> The level of central segregation of Blue Straggler stars proved to be an excellent tracer of the dynamical evolution of old star clusters (the so-called "dynamical clock"), both in the Milky Way and in the Large Magellanic Cloud. The $A^{+}$ parameter, used to measure the Blue Stragglers degree of segregation, has in fact been found to strongly correlate with the parent cluster central relaxation time. Here we studied the Blue-Straggler population of two young stellar systems in the Small Magellanic Cloud, namely NGC 339 (which is 6 Gyr old) and NGC 419 (with an age of only 1.5 Gyr), in order to study their dynamical state. Thanks to multi-epoch, high angular resolution Hubble Space Telescope observations available for both clusters, we took advantage of the stellar proper motions measured in the regions of the two systems and we selected a population of likely cluster members, removing the strong contamination from Small Magellanic Cloud stars. This enabled us to study, with unprecedented accuracy, the radial distribution of Blue Stragglers in these two extragalactic clusters and to measure their dynamical age. As expected for such young clusters, we found that both systems are poorly evolved from the dynamical point of view, also fully confirming that the $A^{+}$ parameter is a sensitive "clock hand" even in the dynamically-young regime. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.07677v1-abstract-full').style.display = 'none'; document.getElementById('2202.07677v1-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">12 pages,11 figures, Accepted for publication by ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2202.01599">arXiv:2202.01599</a> <span> [<a href="https://arxiv.org/pdf/2202.01599">pdf</a>, <a href="https://arxiv.org/format/2202.01599">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="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stac1337">10.1093/mnras/stac1337 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Stellar graveyards: Clustering of compact objects in globular clusters NGC 3201 and NGC 6397 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vitral%2C+E">Eduardo Vitral</a>, <a href="/search/astro-ph?searchtype=author&query=Kremer%2C+K">Kyle Kremer</a>, <a href="/search/astro-ph?searchtype=author&query=Libralato%2C+M">Mattia Libralato</a>, <a href="/search/astro-ph?searchtype=author&query=Mamon%2C+G+A">Gary A. Mamon</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">Andrea Bellini</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="2202.01599v2-abstract-short" style="display: inline;"> We analyse Gaia EDR3 and re-calibrated HST proper motion data from the core-collapsed and non core-collapsed globular clusters NGC 6397 and NGC 3201, respectively, with the Bayesian mass-orbit modelling code MAMPOSSt-PM. We use Bayesian evidence and realistic mock data sets constructed with AGAMA to select between different mass models. In both clusters, the velocities are consistent with isotropy… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.01599v2-abstract-full').style.display = 'inline'; document.getElementById('2202.01599v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.01599v2-abstract-full" style="display: none;"> We analyse Gaia EDR3 and re-calibrated HST proper motion data from the core-collapsed and non core-collapsed globular clusters NGC 6397 and NGC 3201, respectively, with the Bayesian mass-orbit modelling code MAMPOSSt-PM. We use Bayesian evidence and realistic mock data sets constructed with AGAMA to select between different mass models. In both clusters, the velocities are consistent with isotropy within the extent of our data. We robustly detect a dark central mass (DCM) of roughly 1000 solar masses in both clusters. Our MAMPOSSt-PM fits strongly prefer an extended DCM in NGC 6397, while only presenting a mild preference for it in NGC 3201, with respective sizes of a roughly one and a few per cent of the cluster effective radius. We explore the astrophysics behind our results with the CMC Monte Carlo N-body code, whose snapshots best matching the phase space observations lead to similar values for the mass and size of the DCM. The internal kinematics are thus consistent with a population of hundreds of massive white dwarfs in NGC 6397, and roughly 100 segregated stellar-mass black holes in NGC 3201, as previously found with CMC. Such analyses confirm the accuracy of both mass-orbit modelling and Monte Carlo N-body techniques, which together provide more robust predictions on the DCM of globular clusters (core-collapsed or not). This opens possibilities to understand a vast range of interesting astrophysical phenomena in clusters, such as fast radio bursts, compact object mergers, and gravitational waves. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.01599v2-abstract-full').style.display = 'none'; document.getElementById('2202.01599v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">28 pages, 16 figures, 4 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/2201.13296">arXiv:2201.13296</a> <span> [<a href="https://arxiv.org/pdf/2201.13296">pdf</a>, <a href="https://arxiv.org/format/2201.13296">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac739e">10.3847/1538-4357/ac739e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An Isolated Stellar-Mass Black Hole Detected Through Astrometric Microlensing </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sahu%2C+K+C">Kailash C. Sahu</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">Jay Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Casertano%2C+S">Stefano Casertano</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+H+E">Howard E. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">Andrzej Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Dominik%2C+M">Martin Dominik</a>, <a href="/search/astro-ph?searchtype=author&query=Calamida%2C+A">Annalisa Calamida</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">Andrea Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+T+M">Thomas M. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">Marina Rejkuba</a>, <a href="/search/astro-ph?searchtype=author&query=Bajaj%2C+V">Varun Bajaj</a>, <a href="/search/astro-ph?searchtype=author&query=Kains%2C+N">Noe Kains</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+H+C">Henry C. Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Fryer%2C+C+L">Chris L. Fryer</a>, <a href="/search/astro-ph?searchtype=author&query=Yock%2C+P">Philip Yock</a>, <a href="/search/astro-ph?searchtype=author&query=Mroz%2C+P">Przemek Mroz</a>, <a href="/search/astro-ph?searchtype=author&query=Kozlowski%2C+S">Szymon Kozlowski</a>, <a href="/search/astro-ph?searchtype=author&query=Pietrukowicz%2C+P">Pawel Pietrukowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Poleski%2C+R">Radek Poleski</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+J">Jan Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Soszynski%2C+I">Igor Soszynski</a>, <a href="/search/astro-ph?searchtype=author&query=Szymanski%2C+M+K">Michael K. Szymanski</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">Krzysztof Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Wyrzykowski%2C+L">Lukasz Wyrzykowski</a>, <a href="/search/astro-ph?searchtype=author&query=Barry%2C+R">Richard Barry</a> , et al. (68 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="2201.13296v4-abstract-short" style="display: inline;"> We report the first unambiguous detection and mass measurement of an isolated stellar-mass black hole (BH). We used the Hubble Space Telescope (HST) to carry out precise astrometry of the source star of the long-duration (t_E~270 days), high-magnification microlensing event MOA-2011-BLG-191/OGLE-2011-BLG-0462 (hereafter designated as MOA-11-191/OGLE-11-462), in the direction of the Galactic bulge.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.13296v4-abstract-full').style.display = 'inline'; document.getElementById('2201.13296v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.13296v4-abstract-full" style="display: none;"> We report the first unambiguous detection and mass measurement of an isolated stellar-mass black hole (BH). We used the Hubble Space Telescope (HST) to carry out precise astrometry of the source star of the long-duration (t_E~270 days), high-magnification microlensing event MOA-2011-BLG-191/OGLE-2011-BLG-0462 (hereafter designated as MOA-11-191/OGLE-11-462), in the direction of the Galactic bulge. HST imaging, conducted at eight epochs over an interval of six years, reveals a clear relativistic astrometric deflection of the background star's apparent position. Ground-based photometry of MOA-11-191/OGLE-11-462 shows a parallactic signature of the effect of the Earth's motion on the microlensing light curve. Combining the HST astrometry with the ground-based light curve and the derived parallax, we obtain a lens mass of 7.1 +/- 1.3 Msun and a distance of 1.58 +/- 0.18 kpc. We show that the lens emits no detectable light, which, along with having a mass higher than is possible for a white dwarf or neutron star, confirms its BH nature. Our analysis also provides an absolute proper motion for the BH. The proper motion is offset from the mean motion of Galactic-disk stars at similar distances by an amount corresponding to a transverse space velocity of ~45 km/s, suggesting that the BH received a 'natal kick' from its supernova explosion. Previous mass determinations for stellar-mass BHs have come from radial-velocity measurements of Galactic X-ray binaries, and from gravitational radiation emitted by merging BHs in binary systems in external galaxies. Our mass measurement is the first for an isolated stellar-mass BH using any technique. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.13296v4-abstract-full').style.display = 'none'; document.getElementById('2201.13296v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 31 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">37 pages, Published in ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ, 933, 83 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.08631">arXiv:2201.08631</a> <span> [<a href="https://arxiv.org/pdf/2201.08631">pdf</a>, <a href="https://arxiv.org/format/2201.08631">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac5046">10.3847/1538-4357/ac5046 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Survey of multiple populations in globular clusters among very low-mass stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dondoglio%2C+E">E. Dondoglio</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=Renzini%2C+A">A. Renzini</a>, <a href="/search/astro-ph?searchtype=author&query=Vesperini%2C+E">E. Vesperini</a>, <a href="/search/astro-ph?searchtype=author&query=Lagioia%2C+E+P">E. P. Lagioia</a>, <a href="/search/astro-ph?searchtype=author&query=Marino%2C+A+F">A. F. Marino</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">A. Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Carlos%2C+M">M. Carlos</a>, <a href="/search/astro-ph?searchtype=author&query=Cordoni%2C+G">G. Cordoni</a>, <a href="/search/astro-ph?searchtype=author&query=Jang%2C+S">S. Jang</a>, <a href="/search/astro-ph?searchtype=author&query=Legnardi%2C+M+V">M. V. Legnardi</a>, <a href="/search/astro-ph?searchtype=author&query=Libralato%2C+M">M. Libralato</a>, <a href="/search/astro-ph?searchtype=author&query=Mohandasan%2C+A">A. Mohandasan</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Antona%2C+F">F. D'Antona</a>, <a href="/search/astro-ph?searchtype=author&query=Martorano%2C+M">M. Martorano</a>, <a href="/search/astro-ph?searchtype=author&query=Muratore%2C+F">F. Muratore</a>, <a href="/search/astro-ph?searchtype=author&query=Tailo%2C+M">M. Tailo</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="2201.08631v1-abstract-short" style="display: inline;"> Recent work has shown that NIR Hubble Space Telescope (HST) photometry allows us to disentangle multiple populations (MPs) among M dwarfs of globular clusters (GCs) and investigate this phenomenon in very low-mass (VLM) stars. Here, we present the color-magnitude diagrams (CMDs) of nine GCs and the open cluster NGC 6791 in the F110W and F160W bands of HST, showing that the main sequences (MSs) bel… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.08631v1-abstract-full').style.display = 'inline'; document.getElementById('2201.08631v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.08631v1-abstract-full" style="display: none;"> Recent work has shown that NIR Hubble Space Telescope (HST) photometry allows us to disentangle multiple populations (MPs) among M dwarfs of globular clusters (GCs) and investigate this phenomenon in very low-mass (VLM) stars. Here, we present the color-magnitude diagrams (CMDs) of nine GCs and the open cluster NGC 6791 in the F110W and F160W bands of HST, showing that the main sequences (MSs) below the knee are either broadened or split thus providing evidence of MPs among VLM stars. In contrast, the MS of NGC 6791 is consistent with a single population. The color distribution of M-dwarfs dramatically changes between different GCs and the color width correlates with the cluster mass. We conclude that the MP ubiquity, variety, and dependence on GC mass are properties common to VLM and more-massive stars. We combined UV, optical, and NIR observations of NGC 2808 and NGC 6121 (M 4) to identify MPs along with a wide range of stellar masses (~ 0.2 - 0.8M ), from the MS turn off to the VLM regime, and measured, for the first time, their mass functions (MFs). We find that the fraction of MPs does not depend on the stellar mass and that their MFs have similar slopes. These findings indicate that the properties of MPs do not depend on stellar mass. In a scenario where the second generations formed in higher-density environments than the first generations, the possibility that the MPs formed with the same initial MF would suggest that it does not depend on the environment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.08631v1-abstract-full').style.display = 'none'; document.getElementById('2201.08631v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">22 pages, 15 figures. Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.08708">arXiv:2109.08708</a> <span> [<a href="https://arxiv.org/pdf/2109.08708">pdf</a>, <a href="https://arxiv.org/format/2109.08708">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/10.3847/1538-3881/ac281f">10.3847/1538-3881/ac281f <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Relative Ages of Nine Inner Milky Way Globular Clusters from Proper Motion Cleaned Color-Magnitude Diagrams </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R+E">Roger E. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">Andrea Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Casagrande%2C+L">Luca Casagrande</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+T+M">Thomas M. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Correnti%2C+M">Matteo Correnti</a>, <a href="/search/astro-ph?searchtype=author&query=Kalirai%2C+J+S">Jason S. Kalirai</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2109.08708v1-abstract-short" style="display: inline;"> Our picture of the age-metallicity relation for Milky Way globular clusters (MWGCs) is still highly incomplete, and the majority of MWGCs lack self-consistent age measurements. Here, we exploit deep, homogenous multi-epoch Hubble Space Telescope (HST) imaging of nine MWGCs located towards the inner Milky Way to measure their relative ages, in most cases for the first time. Our relative age measure… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.08708v1-abstract-full').style.display = 'inline'; document.getElementById('2109.08708v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.08708v1-abstract-full" style="display: none;"> Our picture of the age-metallicity relation for Milky Way globular clusters (MWGCs) is still highly incomplete, and the majority of MWGCs lack self-consistent age measurements. Here, we exploit deep, homogenous multi-epoch Hubble Space Telescope (HST) imaging of nine MWGCs located towards the inner Milky Way to measure their relative ages, in most cases for the first time. Our relative age measurements are designed to be directly comparable to the large set of MWGC ages presented by VandenBerg et al. (2013, V13), using identical filters, evolutionary models, and bolometric corrections, extended to the higher extinction values relevant to our target clusters. Adopting the V13 MWGC age scale, our relative age measurements imply that our target clusters are consistently very old, with a mean age of 12.9$\pm$0.4 Gyr, with the exception of the young metal-rich MWGC NGC 6342. We perform two tests to validate the precision of our methodology, and discuss the implications of our target cluster loci in the MWGC age-metallicity plane. In addition, we use our fully self-consistent bolometric corrections to assess the systematic impact of variations in the total-to-selective extinction ratio $R_{V}$ on relative age measurements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.08708v1-abstract-full').style.display = 'none'; document.getElementById('2109.08708v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">AJ Accepted. 15 pages, 5 figures, 3 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.08726">arXiv:2107.08726</a> <span> [<a href="https://arxiv.org/pdf/2107.08726">pdf</a>, <a href="https://arxiv.org/ps/2107.08726">ps</a>, <a href="https://arxiv.org/format/2107.08726">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stab1476">10.1093/mnras/stab1476 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The HST large programme on omega Centauri -- IV. catalogue of two external fields </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Scalco%2C+M">M. Scalco</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">A. Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Bedin%2C+L+R">L. R. Bedin</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Libralato%2C+M">M. Libralato</a>, <a href="/search/astro-ph?searchtype=author&query=Salaris%2C+M">M. Salaris</a>, <a href="/search/astro-ph?searchtype=author&query=Vesperini%2C+E">E. Vesperini</a>, <a href="/search/astro-ph?searchtype=author&query=Nardiello%2C+D">D. Nardiello</a>, <a href="/search/astro-ph?searchtype=author&query=Apai%2C+D">D. Apai</a>, <a href="/search/astro-ph?searchtype=author&query=Burgasser%2C+A+J">A. J. Burgasser</a>, <a href="/search/astro-ph?searchtype=author&query=Gerasimov%2C+R">R. Gerasimov</a>, <a href="/search/astro-ph?searchtype=author&query=."> .</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="2107.08726v1-abstract-short" style="display: inline;"> In the fourth paper of this series, we present -- and publicly release -- the state-of-the-art catalogue and atlases for the two remaining parallel fields observed with the Hubble Space Telescope for the large programme on omega Centauri. These two fields are located at ~12' from the centre of the globular cluster (in the West and South-West directions) and were imaged in filters from the ultravio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.08726v1-abstract-full').style.display = 'inline'; document.getElementById('2107.08726v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.08726v1-abstract-full" style="display: none;"> In the fourth paper of this series, we present -- and publicly release -- the state-of-the-art catalogue and atlases for the two remaining parallel fields observed with the Hubble Space Telescope for the large programme on omega Centauri. These two fields are located at ~12' from the centre of the globular cluster (in the West and South-West directions) and were imaged in filters from the ultraviolet to the infrared. Both fields were observed at two epochs separated by about 2 years that were used to derive proper motions and to compute membership probabilities. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.08726v1-abstract-full').style.display = 'none'; document.getElementById('2107.08726v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 11 figures (low resolution). Electronic on-line material at this url https://web.oapd.inaf.it/bedin/files/PAPERs_eMATERIALs/wCen_HST_LargeProgram/P04/ ; Accepted for publication in MNRAS on 2021 May 18th, available at this url https://ui.adsabs.harvard.edu/abs/2021MNRAS.505.3549S/abstract</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> MNRAS.505.3549S (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.02246">arXiv:2105.02246</a> <span> [<a href="https://arxiv.org/pdf/2105.02246">pdf</a>, <a href="https://arxiv.org/format/2105.02246">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/stab1257">10.1093/mnras/stab1257 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> 3D core kinematics of NGC$~$6362: central rotation in a dynamically evolved globular cluster </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dalessandro%2C+E">E. Dalessandro</a>, <a href="/search/astro-ph?searchtype=author&query=Raso%2C+S">S. Raso</a>, <a href="/search/astro-ph?searchtype=author&query=Kamann%2C+S">S. Kamann</a>, <a href="/search/astro-ph?searchtype=author&query=Bellazzini%2C+M">M. Bellazzini</a>, <a href="/search/astro-ph?searchtype=author&query=Vesperini%2C+E">E. Vesperini</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">A. Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Beccari%2C+G">G. Beccari</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2105.02246v1-abstract-short" style="display: inline;"> We present a detailed 3D kinematic analysis of the central regions ($R<30''$) of the low-mass and dynamically evolved galactic globular cluster NGC 6362. The study is based on data obtained with ESO-VLT/MUSE used in combination with the adaptive optics module and providing $\sim3000$ line-of-sight radial velocities, which have been complemented with Hubble Space Telescope proper motions. The quali… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.02246v1-abstract-full').style.display = 'inline'; document.getElementById('2105.02246v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.02246v1-abstract-full" style="display: none;"> We present a detailed 3D kinematic analysis of the central regions ($R<30''$) of the low-mass and dynamically evolved galactic globular cluster NGC 6362. The study is based on data obtained with ESO-VLT/MUSE used in combination with the adaptive optics module and providing $\sim3000$ line-of-sight radial velocities, which have been complemented with Hubble Space Telescope proper motions. The quality of the data and the number of available radial velocities allowed us to detect for the first time a significant rotation signal along the line of sight in the cluster core with amplitude of $\sim 1$ km/s and with a peak located at only $\sim20''$ from the cluster center, corresponding to only $\sim10\%$ of the cluster half-light radius. This result is further supported by the detection of a central and significant tangential anisotropy in the cluster innermost regions. This is one of the most central rotation signals ever observed in a globular cluster to date. We also explore the rotational properties of the multiple populations hosted by this cluster and find that Na-rich stars rotate about two times more rapidly than the Na-poor sub-population thus suggesting that the interpretation of the present-day globular cluster properties require a multi-component chemo-dynamical approach. Both the rotation amplitude and peak position would fit qualitatively the theoretical expectations for a system that lost a significant fraction of its original mass because of the long-term dynamical evolution and interaction with the Galaxy. However, to match the observations more quantitatively further theoretical studies to explore the initial dynamical properties of the cluster are needed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.02246v1-abstract-full').style.display = 'none'; document.getElementById('2105.02246v1-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 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">13 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/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/2101.10751">arXiv:2101.10751</a> <span> [<a href="https://arxiv.org/pdf/2101.10751">pdf</a>, <a href="https://arxiv.org/ps/2101.10751">ps</a>, <a href="https://arxiv.org/format/2101.10751">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/stab233">10.1093/mnras/stab233 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The wide upper main sequence and main sequence turnoff of the ~ 800 Myr old star cluster NGC1831 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Correnti%2C+M">Matteo Correnti</a>, <a href="/search/astro-ph?searchtype=author&query=Goudfrooij%2C+P">Paul Goudfrooij</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">Andrea Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Girardi%2C+L">Leo Girardi</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2101.10751v1-abstract-short" style="display: inline;"> We present the analysis of the colour-magnitude diagram (CMD) morphology of the ~ 800 Myr old star cluster NGC1831 in the Large Magellanic Cloud, exploiting deep, high-resolution photometry obtained using the Wide Field Camera 3 onboard the Hubble Space Telescope. We perform a simultaneous analysis of the wide upper main sequence and main sequence turn-off observed in the cluster, to verify whethe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.10751v1-abstract-full').style.display = 'inline'; document.getElementById('2101.10751v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.10751v1-abstract-full" style="display: none;"> We present the analysis of the colour-magnitude diagram (CMD) morphology of the ~ 800 Myr old star cluster NGC1831 in the Large Magellanic Cloud, exploiting deep, high-resolution photometry obtained using the Wide Field Camera 3 onboard the Hubble Space Telescope. We perform a simultaneous analysis of the wide upper main sequence and main sequence turn-off observed in the cluster, to verify whether these features are due to an extended star formation or a range of stellar rotation rates, or a combination of these two effects. Comparing the observed CMD with Monte Carlo simulations of synthetic stellar populations, we derive that the morphology of NGC1831 can be fully explained in the context of the rotation velocity scenario, under the assumption of a bimodal distribution for the rotating stars, with ~40% of stars being slow-rotators ($惟$ / $惟_{crit}$ < 0.5) and the remaining ~ 60% being fast rotators ($惟$ / $惟_{crit}$ > 0.9). We derive the dynamical properties of the cluster, calculating the present cluster mass and escape velocity, and predicting their past evolution starting at an age of 10 Myr. We find that NGC1831 has an escape velocity $v_{esc}$ = 18.4 km/s, at an age of 10 Myr, above the previously suggested threshold of 15 km/s, below which the cluster cannot retain the material needed to create second-generation stars. These results, combined with those obtained from the CMD morphology analysis, indicate that for the clusters whose morphology cannot be easily explained only in the context of the rotation velocity scenario, the threshold limit should be at least ~ 20 km/s. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.10751v1-abstract-full').style.display = 'none'; document.getElementById('2101.10751v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 10, 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/2012.00791">arXiv:2012.00791</a> <span> [<a href="https://arxiv.org/pdf/2012.00791">pdf</a>, <a href="https://arxiv.org/format/2012.00791">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/10.3847/1538-3881/abd036">10.3847/1538-3881/abd036 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Structure and Internal Kinematics of Nine Inner Milky Way Globular Clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R+E">Roger E. Cohen</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=Correnti%2C+M">Matteo Correnti</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+T+M">Thomas M. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Kalirai%2C+J+S">Jason S. Kalirai</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2012.00791v1-abstract-short" style="display: inline;"> This study constitutes part of a larger effort aimed at better characterizing the Galactic globular clusters (GGCs) located towards the inner Milky Way bulge and disk. Here, we focus on internal kinematics of nine GGCs, obtained from space-based imaging over time baselines of $>$9 years. We exploit multiple avenues to assess the dynamical state of the target GGCs, constructing radial profiles of p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.00791v1-abstract-full').style.display = 'inline'; document.getElementById('2012.00791v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.00791v1-abstract-full" style="display: none;"> This study constitutes part of a larger effort aimed at better characterizing the Galactic globular clusters (GGCs) located towards the inner Milky Way bulge and disk. Here, we focus on internal kinematics of nine GGCs, obtained from space-based imaging over time baselines of $>$9 years. We exploit multiple avenues to assess the dynamical state of the target GGCs, constructing radial profiles of projected stellar density, proper motion dispersion, and anisotropy. We posit that two-thirds (6/9) of our target GGCs are in an advanced dynamical state, and are close to (or have recently undergone) core collapse, supported by at least two lines of evidence: First, we find relatively steep proper motion dispersion profiles, in accord with literature values for core-collapsed GGCs. Second, we find that our sample is, in the mean, isotropic even out to their half-light radii, although one of our target clusters (NGC 6380) is tangentially anisotropic at $>$1$蟽$ beyond its half-light radius, in accord with theoretical predictions for clusters evolving in strong tidal fields. Our proper motion dispersion and anisotropy profiles are made publicly available. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.00791v1-abstract-full').style.display = 'none'; document.getElementById('2012.00791v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">AJ 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/2011.03288">arXiv:2011.03288</a> <span> [<a href="https://arxiv.org/pdf/2011.03288">pdf</a>, <a href="https://arxiv.org/format/2011.03288">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/10.1093/mnras/staa3497">10.1093/mnras/staa3497 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Kinematic complexity around NGC$\,$419: resolving the proper motion of the cluster, the Small Magellanic Cloud and the Magellanic Bridge </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Massari%2C+D">Davide Massari</a>, <a href="/search/astro-ph?searchtype=author&query=Raso%2C+S">Silvia Raso</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> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2011.03288v1-abstract-short" style="display: inline;"> We present $\it{Hubble}$ $\it{Space}$ $\it{Telescope}$ proper motions in the direction of the star cluster NGC$\,$419 in the Small Magellanic Cloud. Because of the high precision of our measurements, for the first time it is possible to resolve the complex kinematics of the stellar populations located in the field, even along the tangential direction. In fact, the proper motions we measured allow… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.03288v1-abstract-full').style.display = 'inline'; document.getElementById('2011.03288v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.03288v1-abstract-full" style="display: none;"> We present $\it{Hubble}$ $\it{Space}$ $\it{Telescope}$ proper motions in the direction of the star cluster NGC$\,$419 in the Small Magellanic Cloud. Because of the high precision of our measurements, for the first time it is possible to resolve the complex kinematics of the stellar populations located in the field, even along the tangential direction. In fact, the proper motions we measured allow us to separate cluster stars, which move on average with ($渭_伪\cos未^{\rm NGC\,419}, 渭_未^{\rm NGC\,419}$) = ($+0.878\pm0.055$, $-1.246\pm0.048$) mas yr$^{-1}$, from those of the Small Magellanic Cloud and those belonging to a third kinematic feature that we recognise as part of the Magellanic Bridge. Resolving such a kinematic complexity enables the construction of decontaminated colour-magnitude diagrams, as well as the measurement of the absolute proper motion of the three separate components. Our study therefore sets the first steps towards the possibility of dynamically investigating the Magellanic system by exploiting the resolved kinematics of its stellar clusters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.03288v1-abstract-full').style.display = 'none'; document.getElementById('2011.03288v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 9 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/2010.10964">arXiv:2010.10964</a> <span> [<a href="https://arxiv.org/pdf/2010.10964">pdf</a>, <a href="https://arxiv.org/format/2010.10964">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/staa3329">10.1093/mnras/staa3329 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> 2D kinematics of massive stars near the Galactic Center </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Libralato%2C+M">Mattia Libralato</a>, <a href="/search/astro-ph?searchtype=author&query=Lennon%2C+D+J">Daniel J. Lennon</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">Andrea Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Marel%2C+R">Roeland van der Marel</a>, <a href="/search/astro-ph?searchtype=author&query=Clark%2C+S+J">Simon J. Clark</a>, <a href="/search/astro-ph?searchtype=author&query=Najarro%2C+F">Francisco Najarro</a>, <a href="/search/astro-ph?searchtype=author&query=Patrick%2C+L+R">Lee R. Patrick</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">Jay Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Bedin%2C+L+R">Luigi R. Bedin</a>, <a href="/search/astro-ph?searchtype=author&query=Crowther%2C+P+A">Paul A. Crowther</a>, <a href="/search/astro-ph?searchtype=author&query=de+Mink%2C+S+E">Selma E. de Mink</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+C+J">Christopher J. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Platais%2C+I">Imants Platais</a>, <a href="/search/astro-ph?searchtype=author&query=Sabbi%2C+E">Elena Sabbi</a>, <a href="/search/astro-ph?searchtype=author&query=Sohn%2C+S+T">Sangmo Tony Sohn</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2010.10964v2-abstract-short" style="display: inline;"> The presence of massive stars (MSs) in the region close to the Galactic Center (GC) poses several questions about their origin. The harsh environment of the GC favors specific formation scenarios, each of which should imprint characteristic kinematic features on the MSs. We present a 2D kinematic analysis of MSs in a GC region surrounding Sgr A* based on high-precision proper motions obtained with… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.10964v2-abstract-full').style.display = 'inline'; document.getElementById('2010.10964v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.10964v2-abstract-full" style="display: none;"> The presence of massive stars (MSs) in the region close to the Galactic Center (GC) poses several questions about their origin. The harsh environment of the GC favors specific formation scenarios, each of which should imprint characteristic kinematic features on the MSs. We present a 2D kinematic analysis of MSs in a GC region surrounding Sgr A* based on high-precision proper motions obtained with the Hubble Space Telescope. Thanks to a careful data reduction, well-measured bright stars in our proper-motion catalogs have errors better than 0.5 mas yr$^{-1}$. We discuss the absolute motion of the MSs in the field and their motion relative to Sgr A*, the Arches and the Quintuplet. For the majority of the MSs, we rule out any distance further than 3-4 kpc from Sgr A* using only kinematic arguments. If their membership to the GC is confirmed, most of the isolated MSs are likely not associated with either the Arches or Quintuplet clusters or Sgr A*. Only a few MSs have proper motions suggesting they are likely members of the Arches cluster, in agreement with previous spectroscopic results. Line-of-sight radial velocities and distances are required to shed further light on the origin of most of these massive objects. We also present an analysis of other fast-moving objects in the GC region, finding no clear excess of high-velocity escaping stars. We make our astro-photometric catalogs publicly available. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.10964v2-abstract-full').style.display = 'none'; document.getElementById('2010.10964v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages, 33 figures, 9 tables. Accepted for publication in MNRAS. [v3: Fixed bibliography]</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2008.01741">arXiv:2008.01741</a> <span> [<a href="https://arxiv.org/pdf/2008.01741">pdf</a>, <a href="https://arxiv.org/format/2008.01741">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/staa2327">10.1093/mnras/staa2327 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The absolute proper motions of the Arches and Quintuplet clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Libralato%2C+M">M. Libralato</a>, <a href="/search/astro-ph?searchtype=author&query=Fardal%2C+M">M. Fardal</a>, <a href="/search/astro-ph?searchtype=author&query=Lennon%2C+D">D. Lennon</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Marel%2C+R+P">R. P. van der Marel</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">A. Bellini</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2008.01741v2-abstract-short" style="display: inline;"> Arches and Quintuplet are two young, massive clusters projected near the Galactic Center. To date, studies focused on understanding their origin have been based on proper motions (PMs) derived in the clusters' reference frames and required some assumptions about their 3D motion. In this paper, we combine public PM catalogs of these clusters with the Gaia DR2 catalog and, for the first time, transf… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.01741v2-abstract-full').style.display = 'inline'; document.getElementById('2008.01741v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.01741v2-abstract-full" style="display: none;"> Arches and Quintuplet are two young, massive clusters projected near the Galactic Center. To date, studies focused on understanding their origin have been based on proper motions (PMs) derived in the clusters' reference frames and required some assumptions about their 3D motion. In this paper, we combine public PM catalogs of these clusters with the Gaia DR2 catalog and, for the first time, transform the relative PMs of the Arches and Quintuplet clusters onto an absolute reference system. We find that the absolute PM of the Arches is $(渭_伪\cos未,渭_未)$ $=$ $(-1.45\ \pm\ 0.23,-2.68\ \pm\ 0.14)$ mas yr$^{-1}$, and that of the Quintuplet is $(渭_伪\cos未,渭_未)$ $=$ $(-1.19\ \pm\ 0.09,-2.66\ \pm \ 0.18)$ mas yr$^{-1}$. These values suggest that these systems are moving almost parallel to the Galactic plane. A measurement of the clusters' distances is still required to meaningfully constrain the clusters' orbits and shed light on the origin of the Arches and Quintuplet. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.01741v2-abstract-full').style.display = 'none'; document.getElementById('2008.01741v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 8 figures, accepted for publication in MNRAS. v2: Fixed Bibliography</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2004.14472">arXiv:2004.14472</a> <span> [<a href="https://arxiv.org/pdf/2004.14472">pdf</a>, <a href="https://arxiv.org/ps/2004.14472">ps</a>, <a href="https://arxiv.org/format/2004.14472">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/ab8d42">10.3847/1538-3881/ab8d42 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> HST astrometry in the Orion Nebula Cluster: census of low-mass runaways </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Platais%2C+I">Imants Platais</a>, <a href="/search/astro-ph?searchtype=author&query=Robberto%2C+M">Massimo Robberto</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">Andrea Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Kozhurina-Platais%2C+V">Vera Kozhurina-Platais</a>, <a href="/search/astro-ph?searchtype=author&query=Gennaro%2C+M">Mario Gennaro</a>, <a href="/search/astro-ph?searchtype=author&query=Strampelli%2C+G">Giovanni Strampelli</a>, <a href="/search/astro-ph?searchtype=author&query=Hillenbrand%2C+L+A">Lynne A. Hillenbrand</a>, <a href="/search/astro-ph?searchtype=author&query=de+Mink%2C+S+E">Selma E. de Mink</a>, <a href="/search/astro-ph?searchtype=author&query=Soderblom%2C+D+R">David R. Soderblom</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2004.14472v1-abstract-short" style="display: inline;"> We present a catalog of high-precision proper motions in the Orion Nebula Cluster (ONC), based on Treasury Program observations with the Hubble Space Telescope's (HST) ACS/WFC camera. Our catalog contains 2,454 objects in the magnitude range of $14.2<m_{\rm F775W}<24.7$, thus probing the stellar masses of the ONC from $\sim$0.4 $M_\odot$ down to $\sim$0.02 $M_\odot$ over an area of $\sim$550 arcmi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.14472v1-abstract-full').style.display = 'inline'; document.getElementById('2004.14472v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2004.14472v1-abstract-full" style="display: none;"> We present a catalog of high-precision proper motions in the Orion Nebula Cluster (ONC), based on Treasury Program observations with the Hubble Space Telescope's (HST) ACS/WFC camera. Our catalog contains 2,454 objects in the magnitude range of $14.2<m_{\rm F775W}<24.7$, thus probing the stellar masses of the ONC from $\sim$0.4 $M_\odot$ down to $\sim$0.02 $M_\odot$ over an area of $\sim$550 arcmin$^2$. We provide a number of internal velocity dispersion estimates for the ONC that indicate a weak dependence on the stellar location and mass. There is good agreement with the published velocity dispersion estimates, although nearly all of them (including ours at $蟽_{v,x}=0.94$ and $蟽_{v,y}=1.25$ mas yr$^{-1}$) might be biased by the overlapping young stellar populations of Orion A. We identified 4 new ONC candidate runaways based on HST and the Gaia DR2 data, all with masses less than $\sim$1 $M_\odot$. The total census of known candidate runaway sources is 10 -- one of the largest samples ever found in any Milky Way open star cluster. Surprisingly, none of them has the tangential velocity exceeding 20 km s$^{-1}$. If most of them indeed originated in the ONC, it may compel re-examination of dynamical processes in very young star clusters. It appears that the mass function of the ONC is not significantly affected by the lost runaways. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.14472v1-abstract-full').style.display = 'none'; document.getElementById('2004.14472v1-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 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 10 figures, 5 tables. Accepted for publication in 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/2004.13915">arXiv:2004.13915</a> <span> [<a href="https://arxiv.org/pdf/2004.13915">pdf</a>, <a href="https://arxiv.org/format/2004.13915">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ab911e">10.3847/1538-4357/ab911e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> HST survey of the Orion Nebula Cluster in the H$_2$O 1.4 $渭$m absorption band: I. A census of substellar and planetary mass objects </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Robberto%2C+M">Massimo Robberto</a>, <a href="/search/astro-ph?searchtype=author&query=Gennaro%2C+M">Mario Gennaro</a>, <a href="/search/astro-ph?searchtype=author&query=Gabellini%2C+M+G+U">Maria Giulia Ubeira Gabellini</a>, <a href="/search/astro-ph?searchtype=author&query=Hillenbrand%2C+L+A">Lynne A. Hillenbrand</a>, <a href="/search/astro-ph?searchtype=author&query=Pacifici%2C+C">Camilla Pacifici</a>, <a href="/search/astro-ph?searchtype=author&query=Ubeda%2C+L">Leonardo Ubeda</a>, <a href="/search/astro-ph?searchtype=author&query=Andersen%2C+M">Morten Andersen</a>, <a href="/search/astro-ph?searchtype=author&query=Barman%2C+T">Travis Barman</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">Andrea Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Da+Rio%2C+N">Nicola Da Rio</a>, <a href="/search/astro-ph?searchtype=author&query=de+Mink%2C+S+E">Selma E. de Mink</a>, <a href="/search/astro-ph?searchtype=author&query=Lodato%2C+G">Giuseppe Lodato</a>, <a href="/search/astro-ph?searchtype=author&query=Manara%2C+C+F">Carlo Felice Manara</a>, <a href="/search/astro-ph?searchtype=author&query=Platais%2C+I">Imants Platais</a>, <a href="/search/astro-ph?searchtype=author&query=Pueyo%2C+L">Laurent Pueyo</a>, <a href="/search/astro-ph?searchtype=author&query=Strampelli%2C+G+M">Giovanni M. Strampelli</a>, <a href="/search/astro-ph?searchtype=author&query=Tan%2C+J+C">Jonathan C. Tan</a>, <a href="/search/astro-ph?searchtype=author&query=Testi%2C+L">Leonardo Testi</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2004.13915v1-abstract-short" style="display: inline;"> In order to obtain a complete census of the stellar and sub-stellar population, down to a few M$_{Jup}$ in the $\sim1$ Myr old Orion Nebula Cluster, we used the infrared channel of the Wide Field Camera 3 of the Hubble Space Telescope with the F139M and F130N filters. These bandpasses correspond to the $1.4 渭$m H$_2$O absorption feature and an adjacent line-free continuum region. Out of $4,504$ de… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.13915v1-abstract-full').style.display = 'inline'; document.getElementById('2004.13915v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2004.13915v1-abstract-full" style="display: none;"> In order to obtain a complete census of the stellar and sub-stellar population, down to a few M$_{Jup}$ in the $\sim1$ Myr old Orion Nebula Cluster, we used the infrared channel of the Wide Field Camera 3 of the Hubble Space Telescope with the F139M and F130N filters. These bandpasses correspond to the $1.4 渭$m H$_2$O absorption feature and an adjacent line-free continuum region. Out of $4,504$ detected sources, $3,352$ (about $75\%$) appear fainter than m$_{130}=14$ (Vega mag) in the F130N filter, a brightness corresponding to the hydrogen-burning limit mass (M$\simeq 0.072 M_\odot$) at $\sim 1$ Myr. Of these, however, only $742$ sources have a negative F130M-139N color index, indicative of the presence of H$_2$O vapor in absorption, and can therefore be classified as bona-fide M and L dwarfs, with effective temperatures T$\lesssim 2850$ K at an assumed $1$ Myr cluster age. On our color-magnitude diagram, this population of sources with H$_2$O absorption appears clearly distinct from the larger background population of highly reddened stars and galaxies with positive F130M-F139N color index, and can be traced down to the sensitivity limit of our survey, m$_{130}\simeq 21.5$, corresponding to a $1$ Myr old $\simeq 3 $M$_{Jup}$, planetary mass object under about 2 magnitudes of visual extinction. Theoretical models of the BT-Settl family predicting substellar isochrones of $1, 2$ and $3$ Myr (down to $\sim 1 $M$_{Jup}$) fail to reproduce the observed H$_2$O color index at M$\lesssim 20 $M$_{Jup}$. We perform a Bayesian analysis to determine extinction, mass and effective temperature of each sub-stellar member of our sample, together with its membership probability. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.13915v1-abstract-full').style.display = 'none'; document.getElementById('2004.13915v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in the Astrophysical Journal. The resolution of several figures has been downgraded to comply with the size limit of arXiv submissions</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2004.09540">arXiv:2004.09540</a> <span> [<a href="https://arxiv.org/pdf/2004.09540">pdf</a>, <a href="https://arxiv.org/format/2004.09540">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ab8ae7">10.3847/1538-4357/ab8ae7 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A kinematic view of NGC 1261: structural parameters, internal dispersion, absolute proper motion and Blue Straggler Stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Raso%2C+S">S. Raso</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=Ferraro%2C+F+R">F. R. Ferraro</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzoni%2C+B">B. Lanzoni</a>, <a href="/search/astro-ph?searchtype=author&query=Cadelano%2C+M">M. Cadelano</a>, <a href="/search/astro-ph?searchtype=author&query=Pallanca%2C+C">C. Pallanca</a>, <a href="/search/astro-ph?searchtype=author&query=Dalessandro%2C+E">E. Dalessandro</a>, <a href="/search/astro-ph?searchtype=author&query=Piotto%2C+G">G. Piotto</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Sohn%2C+S+T">S. T. Sohn</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2004.09540v1-abstract-short" style="display: inline;"> We constructed a Hubble Space Telescope (HST) astro-photometric catalog of the central region of the Galactic globular cluster NGC 1261. This catalog, complemented with Gaia DR2 data sampling the external regions, has been used to estimate the structural parameters of the system (i.e., core, half-mass, tidal radii and concentration) from its resolved star density profile. We computed high-precisio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.09540v1-abstract-full').style.display = 'inline'; document.getElementById('2004.09540v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2004.09540v1-abstract-full" style="display: none;"> We constructed a Hubble Space Telescope (HST) astro-photometric catalog of the central region of the Galactic globular cluster NGC 1261. This catalog, complemented with Gaia DR2 data sampling the external regions, has been used to estimate the structural parameters of the system (i.e., core, half-mass, tidal radii and concentration) from its resolved star density profile. We computed high-precision proper motions thanks to multi-epoch HST data and derived the cluster velocity dispersion profile in the plane of the sky for the innermost region, finding that the system is isotropic. The combination with line-of-sight information collected from spectroscopy in the external regions provided us with the cluster velocity dispersion profile along the entire radial extension. We also measured the absolute proper motion of NGC 1261 using a few background galaxies as a reference. The radial distribution of the Blue Straggler Star population shows that the cluster is in a low/intermediate phase of dynamical evolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.09540v1-abstract-full').style.display = 'none'; document.getElementById('2004.09540v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 12 figures, 2 tables; accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2002.11653">arXiv:2002.11653</a> <span> [<a href="https://arxiv.org/pdf/2002.11653">pdf</a>, <a href="https://arxiv.org/format/2002.11653">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/ab8f9e">10.3847/1538-3881/ab8f9e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Proper-Motion Membership Tests for Four Planetary Nebulae in Galactic Globular Clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bond%2C+H+E">Howard E. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">Andrea Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Sahu%2C+K+C">Kailash C. Sahu</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2002.11653v2-abstract-short" style="display: inline;"> Four planetary nebulae (PNe) are considered to be probable or possible members of Galactic globular clusters (GCs). These are Ps 1 = K648 in M15, GJJC 1 = IRAS 18333-2357 in M22, JaFu 1 in Palomar 6, and JaFu 2 in NGC 6441. In addition to lying close to the host GCs on the sky, these PNe have radial velocities that are consistent, within the errors and stellar velocity dispersions, with cluster me… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.11653v2-abstract-full').style.display = 'inline'; document.getElementById('2002.11653v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2002.11653v2-abstract-full" style="display: none;"> Four planetary nebulae (PNe) are considered to be probable or possible members of Galactic globular clusters (GCs). These are Ps 1 = K648 in M15, GJJC 1 = IRAS 18333-2357 in M22, JaFu 1 in Palomar 6, and JaFu 2 in NGC 6441. In addition to lying close to the host GCs on the sky, these PNe have radial velocities that are consistent, within the errors and stellar velocity dispersions, with cluster membership. The remaining membership criterion is whether the proper motions (PMs) of the central stars are in agreement with those of the host clusters. We have carried out the PM test for all four PNe. Two of the central stars--those of Ps 1 and GJJC 1--have PMs listed in the recent Gaia Data Release 2 (DR2). We updated the PM of the Ps 1 central star to a more precise value using archival Hubble Space Telescope (HST) frames. Both PMs are statistically consistent with cluster membership. For the other two PNe, we used archival HST images to derive the PMs of their nuclei. For JaFu 2, there are HST images at several epochs, and the measured PM of the nucleus is in excellent agreement with that of the host cluster. For JaFu 1 the available archival HST images are less optimal and the results are less conclusive; the measured PM for the central star is marginally consistent with cluster membership, but additional astrometric observations are desirable for a more robust membership test. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.11653v2-abstract-full').style.display = 'none'; document.getElementById('2002.11653v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 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">Revised version, accepted by Astronomical Journal</span> </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Bellini%2C+A&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Bellini%2C+A&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Bellini%2C+A&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Bellini%2C+A&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=Bellini%2C+A&start=150" class="pagination-link " aria-label="Page 4" aria-current="page">4 </a> </li> </ul> </nav> <div class="is-hidden-tablet">  <span 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