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</div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.15918">arXiv:2407.15918</a> <span> [<a href="https://arxiv.org/pdf/2407.15918">pdf</a>, <a href="https://arxiv.org/format/2407.15918">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"> Combined Gemini-South and HST photometric analysis of the globular cluster NGC 6558. The age of the metal-poor population of the Galactic Bulge </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Souza%2C+S+O">S. O. Souza</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=Kerber%2C+L+O">L. O. Kerber</a>, <a href="/search/astro-ph?searchtype=author&query=Ortolani%2C+S">S. Ortolani</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A9rez-Villegas%2C+A">A. P茅rez-Villegas</a>, <a href="/search/astro-ph?searchtype=author&query=Oliveira%2C+R+A+P">R. A. P. Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">B. Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=Bica%2C+E">E. Bica</a>, <a href="/search/astro-ph?searchtype=author&query=Griggio%2C+M">M. Griggio</a>, <a href="/search/astro-ph?searchtype=author&query=Dias%2C+B">B. Dias</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="2407.15918v1-abstract-short" style="display: inline;"> NGC~6558 is a low-galactic latitude globular cluster projected in the direction of the Galactic bulge. Due to high reddening, this region presents challenges in deriving accurate parameters, which require meticulous photometric analysis. We present a combined analysis of near-infrared and optical photometry from multi-epoch high-resolution images collected with Gemini-South/GSAOI+GeMS (in the $J$… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.15918v1-abstract-full').style.display = 'inline'; document.getElementById('2407.15918v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.15918v1-abstract-full" style="display: none;"> NGC~6558 is a low-galactic latitude globular cluster projected in the direction of the Galactic bulge. Due to high reddening, this region presents challenges in deriving accurate parameters, which require meticulous photometric analysis. We present a combined analysis of near-infrared and optical photometry from multi-epoch high-resolution images collected with Gemini-South/GSAOI+GeMS (in the $J$ and $K_S$ filters) and HST/ACS (in the F606W and F814W filters). We aim to refine the fundamental parameters of NGC~6558, utilizing high-quality Gemini-South/GSAOI and HST/ACS photometries. Additionally, we intend to investigate its role in the formation of the Galactic bulge. We studied the impact of two differential reddening corrections on the age derivation. When removing as much as possible the Galactic bulge field star contamination, the isochrone fitting combined with synthetic colour-magnitude diagrams gives a distance of $8.41^{+0.11}_{-0.10}$ kpc, an age of $13.0\pm 0.9$ Gyr, a reddening of E($B-V$)$\,\,=0.34\pm0.02$, and a total-to-selective coefficient R$_V = 3.2\pm0.2$ thanks to the simultaneous near-infrared$-$Optical synthetic colour-magnitude diagram fitting. The orbital parameters showed that NGC~6558 is confined whitin the inner Galaxy and it is not compatible with a bar-shape orbit, indicating that it is a bulge member. The old age of NGC~6558, combined with similar metallicity and a blue horizontal branch in the Galactic bulge, indicates that it is part of the moderately metal-poor globular clusters. Assembling the old and moderately metal-poor ([Fe/H]$\,\,\sim-1.1$) clusters in the Galactic bulge, we derived their age-metallicity relation with star formation stars at $13.6\pm0.2$ Gyr and effective yields of $蟻=0.007\pm0.009\,\, Z_\odot$ showing a chemical enrichment ten times faster than the ex-situ globular clusters branch. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.15918v1-abstract-full').style.display = 'none'; document.getElementById('2407.15918v1-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, 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 for publication in A&A. 14 pages, 12 figures, and 4 tables. The abstract is a reduced version of the accepted one</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.03068">arXiv:2405.03068</a> <span> [<a href="https://arxiv.org/pdf/2405.03068">pdf</a>, <a href="https://arxiv.org/format/2405.03068">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/10.1051/0004-6361/202346377">10.1051/0004-6361/202346377 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A census of new globular clusters in the Galactic bulge </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bica%2C+E">E. Bica</a>, <a href="/search/astro-ph?searchtype=author&query=Ortolani%2C+S">S. Ortolani</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">B. Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=Oliveira%2C+R+A+P">R. A. P. Oliveira</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="2405.03068v2-abstract-short" style="display: inline;"> The number of known globular clusters in the Galactic bulge has been increasing steadily thanks to different new surveys. The aim of this study is to provide a census of the newly revealed globular clusters in the Galactic bulge, and analyze their characteristics. In recent years, many globular clusters have been discovered or identified. The stellar populations to which they belong are indicated… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.03068v2-abstract-full').style.display = 'inline'; document.getElementById('2405.03068v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.03068v2-abstract-full" style="display: none;"> The number of known globular clusters in the Galactic bulge has been increasing steadily thanks to different new surveys. The aim of this study is to provide a census of the newly revealed globular clusters in the Galactic bulge, and analyze their characteristics. In recent years, many globular clusters have been discovered or identified. The stellar populations to which they belong are indicated in their original studies: they are mostly bulge clusters, with some identified as disk or halo members. We collected 41 new globular clusters revealed in the last decade and compared them to the known bulge clusters. The new clusters are intrinsically faint with $M_V$ of around -6.0 mag. The distance to the Sun of the ensemble of well-known and new bulge clusters is compatible with the Galactocentric distance measurements from the Galactic black hole location. The ensemble sample shows metallicity peaks at [Fe/H] ~ -1.08 $\pm$ 0.35 and -0.51 $\pm$ 0.25 dex, confirming previous findings. The age-metallicity relation of the new clusters younger than 10 Gyr is compatible with that of the ex situ samples of the dwarf galaxies Sagittarius, Canis Majoris, and Gaia-Enceladus-Sausage. The clusters with ages between 11.5 and 13.5 Gyr show no age-metallicity relation, because they are all old. This is compatible with their formation in situ in the early Galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.03068v2-abstract-full').style.display = 'none'; document.getElementById('2405.03068v2-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 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 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">9 pages, 5 figures. Accepted for publication in A&A. Galactic coordinates of Minni 22 and Gran 5 were corrected in the new version</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.18165">arXiv:2404.18165</a> <span> [<a href="https://arxiv.org/pdf/2404.18165">pdf</a>, <a href="https://arxiv.org/format/2404.18165">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1051/0004-6361/202450535">10.1051/0004-6361/202450535 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> ELEPHANT: ExtragaLactic alErt Pipeline for Hostless AstroNomical Transients </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pessi%2C+P+J">P. J. Pessi</a>, <a href="/search/astro-ph?searchtype=author&query=Durgesh%2C+R">R. Durgesh</a>, <a href="/search/astro-ph?searchtype=author&query=Nakazono%2C+L">L. Nakazono</a>, <a href="/search/astro-ph?searchtype=author&query=Hayes%2C+E+E">E. E. Hayes</a>, <a href="/search/astro-ph?searchtype=author&query=Oliveira%2C+R+A+P">R. A. P. Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Ishida%2C+E+E+O">E. E. O. Ishida</a>, <a href="/search/astro-ph?searchtype=author&query=Moitinho%2C+A">A. Moitinho</a>, <a href="/search/astro-ph?searchtype=author&query=Krone-Martins%2C+A">A. Krone-Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Moews%2C+B">B. Moews</a>, <a href="/search/astro-ph?searchtype=author&query=de+Souza%2C+R+S">R. S. de Souza</a>, <a href="/search/astro-ph?searchtype=author&query=Beck%2C+R">R. Beck</a>, <a href="/search/astro-ph?searchtype=author&query=Kuhn%2C+M+A">M. A. Kuhn</a>, <a href="/search/astro-ph?searchtype=author&query=Nowak%2C+K">K. Nowak</a>, <a href="/search/astro-ph?searchtype=author&query=Vaughan%2C+S">S. Vaughan</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="2404.18165v1-abstract-short" style="display: inline;"> Context. Transient astronomical events that exhibit no discernible association with a host galaxy are commonly referred to as hostless. These rare phenomena are associated with extremely energetic events, and they can offer unique insights into the properties and evolution of stars and galaxies. However, the sheer number of transients captured by contemporary high-cadence astronomical surveys rend… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.18165v1-abstract-full').style.display = 'inline'; document.getElementById('2404.18165v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.18165v1-abstract-full" style="display: none;"> Context. Transient astronomical events that exhibit no discernible association with a host galaxy are commonly referred to as hostless. These rare phenomena are associated with extremely energetic events, and they can offer unique insights into the properties and evolution of stars and galaxies. However, the sheer number of transients captured by contemporary high-cadence astronomical surveys renders the manual identification of all potential hostless transients impractical. Therefore, creating a systematic identification tool is crucial for studying these elusive events. Aims. We present the ExtragaLactic alErt Pipeline for Hostless AstroNomical Transients (ELEPHANT), a framework for filtering hostless transients in astronomical data streams. Methods. We used Fink to access all the ZTF alerts produced between January/2022 and December/2023, selecting only those associated with extragalactic transients. We then processed the associated stamps using a sequence of image analysis techniques to retrieve hostless candidates. Results. We find that less than 2% of all analyzed transients are potentially hostless. Among them, approximately 10% have a spectroscopic class reported on TNS, with Type Ia supernova being the most common class, followed by SLSN. Among the hostless candidates retrieved by our pipeline, there was SN 2018ibb, which has been proposed to be a PISN candidate; and SN 2022ann, one of only five known SNe Icn. When no class is reported on TNS, the dominant classes are QSO and SN candidates, the former obtained from SIMBAD and the latter inferred using the Fink ML classifier. Conclusions. ELEPHANT represents an effective strategy to filter extragalactic events within large and complex astronomical alert streams. There are many applications for which this pipeline will be useful, ranging from transient selection for follow-up to studies of transient environments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.18165v1-abstract-full').style.display = 'none'; document.getElementById('2404.18165v1-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, 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">15 pages, 11 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 691, A181 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.09756">arXiv:2312.09756</a> <span> [<a href="https://arxiv.org/pdf/2312.09756">pdf</a>, <a href="https://arxiv.org/format/2312.09756">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"> The VISCACHA survey -- IX. The SMC Southern Bridge in 8D </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Parisi%2C+M+C">M. C. Parisi</a>, <a href="/search/astro-ph?searchtype=author&query=Oliveira%2C+R+A+P">R. A. P. Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Angelo%2C+M">M. Angelo</a>, <a href="/search/astro-ph?searchtype=author&query=Dias%2C+B">B. Dias</a>, <a href="/search/astro-ph?searchtype=author&query=Maia%2C+F">F. Maia</a>, <a href="/search/astro-ph?searchtype=author&query=Saroon%2C+S">S. Saroon</a>, <a href="/search/astro-ph?searchtype=author&query=Feinstein%2C+C">C. Feinstein</a>, <a href="/search/astro-ph?searchtype=author&query=Santos%2C+J+F+C">J. F. C. Santos Jr.</a>, <a href="/search/astro-ph?searchtype=author&query=Bica%2C+E">E. Bica</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+B+P+L">B. Pereira Lima Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez-Trincado%2C+J+G">J. G. Fern谩ndez-Trincado</a>, <a href="/search/astro-ph?searchtype=author&query=Westera%2C+P">P. Westera</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</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=Santrich%2C+O+J+K">O. J. Katime Santrich</a>, <a href="/search/astro-ph?searchtype=author&query=De+Bortoli%2C+B">B. De Bortoli</a>, <a href="/search/astro-ph?searchtype=author&query=Souza%2C+S">S. Souza</a>, <a href="/search/astro-ph?searchtype=author&query=Kerber%2C+L">L. Kerber</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A9rez-Villegas%2C+A">A. P茅rez-Villegas</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="2312.09756v1-abstract-short" style="display: inline;"> The structure of the Small Magellanic Cloud (SMC) outside of its main body is characterised by tidal branches resulting from its interactions mainly with the Large Magellanic Cloud (LMC). Characterising the stellar populations in these tidal components helps to understand the dynamical history of this galaxy and of the Magellanic system in general. We provide full phase-space vector information fo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.09756v1-abstract-full').style.display = 'inline'; document.getElementById('2312.09756v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.09756v1-abstract-full" style="display: none;"> The structure of the Small Magellanic Cloud (SMC) outside of its main body is characterised by tidal branches resulting from its interactions mainly with the Large Magellanic Cloud (LMC). Characterising the stellar populations in these tidal components helps to understand the dynamical history of this galaxy and of the Magellanic system in general. We provide full phase-space vector information for Southern Bridge clusters. We performed a photometric and spectroscopic analysis of twelve SMC clusters, doubling the number of SMC clusters with full phase-space vector information known to date. We reclassify the sample considering 3D distances and 3D velocities. We found that some of the clusters classified as Southern Bridge objects according to the projected 2D classification actually belong to the Main Body and Counter-Bridge in the background. The comparison of the kinematics of the genuine foreground Bridge clusters with those previously analysed in the same way reveals that Southern Bridge clusters are moving towards the LMC and share the kinematics of the Northern Bridge. Adding to our sample clusters from the literature with CaT metallicity determinations we compare the age-metallicity relation of the Southern Bridge with the one of the Northern Bridge. We reinforce the idea that both regions do not seem to have experienced the same chemical enrichment history and that there is a clear absence of clusters in the Northern Bridge older than 3Gyr and more metal-poor than -1.1, which would not seem to be due to a selection effect. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.09756v1-abstract-full').style.display = 'none'; document.getElementById('2312.09756v1-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, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">18 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/2307.08709">arXiv:2307.08709</a> <span> [<a href="https://arxiv.org/pdf/2307.08709">pdf</a>, <a href="https://arxiv.org/format/2307.08709">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202346648">10.1051/0004-6361/202346648 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The VISCACHA survey -- VIII. Chemical evolution history of Small Magellanic Cloud West Halo cluster </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Saroon%2C+S">S. Saroon</a>, <a href="/search/astro-ph?searchtype=author&query=Dias%2C+B">B. Dias</a>, <a href="/search/astro-ph?searchtype=author&query=Tsujimotto%2C+T">T. Tsujimotto</a>, <a href="/search/astro-ph?searchtype=author&query=Parisi%2C+M+C">M. C. Parisi</a>, <a href="/search/astro-ph?searchtype=author&query=Maia%2C+F">F. Maia</a>, <a href="/search/astro-ph?searchtype=author&query=Kerber%2C+L">L. Kerber</a>, <a href="/search/astro-ph?searchtype=author&query=Bekki%2C+K">K. Bekki</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Oliveira%2C+R+A+P">R. A. P. Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Westera%2C+P">P. Westera</a>, <a href="/search/astro-ph?searchtype=author&query=Santrich%2C+O+J+K">O. J. K. Santrich</a>, <a href="/search/astro-ph?searchtype=author&query=Bica%2C+E">E. Bica</a>, <a href="/search/astro-ph?searchtype=author&query=Sanmartim%2C+D">D. Sanmartim</a>, <a href="/search/astro-ph?searchtype=author&query=Quint%2C+B+C">B. C. Quint</a>, <a href="/search/astro-ph?searchtype=author&query=Fraga%2C+L">L. Fraga</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2307.08709v1-abstract-short" style="display: inline;"> The chemical evolution history of the Small Magellanic Cloud (SMC) has been a matter of debate for decades. The challenges in understanding the SMC chemical evolution are related to a very slow star formation rate (SFR) combined with bursts triggered by the multiple interactions between the SMC and the Large Magellanic Cloud, a significant (~0.5 dex) metallicity dispersion for the SMC cluster popu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.08709v1-abstract-full').style.display = 'inline'; document.getElementById('2307.08709v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.08709v1-abstract-full" style="display: none;"> The chemical evolution history of the Small Magellanic Cloud (SMC) has been a matter of debate for decades. The challenges in understanding the SMC chemical evolution are related to a very slow star formation rate (SFR) combined with bursts triggered by the multiple interactions between the SMC and the Large Magellanic Cloud, a significant (~0.5 dex) metallicity dispersion for the SMC cluster population younger than about 7.5 Gyr, and multiple chemical evolution models tracing very different paths through the observed age-metallicity relation of the SMC. There is no doubt that these processes were complex. Therefore, a step-by-step strategy is required in order to better understand the SMC chemical evolution. We adopted an existing framework to split the SMC into regions on the sky, and we focus on the west halo in this work, which contains the oldest and most metal-poor stellar populations and is moving away from the SMC, that is, in an opposite motion with respect to the Magellanic Bridge. We present a sample containing ~60% of all west halo clusters to represent the region well, and we identify a clear age-metallicity relation with a tight dispersion that exhibits a 0.5 dex metallicity dip about 6 Gyr ago. We ran chemical evolution models and discuss possible scenarios to explain this metallicity dip, the most likely being a major merger accelerating the SFR after the event. This merger should be combined with inefficient internal gas mixing within the SMC and different SFRs in different SMC regions because the same metallicity dip is not seen in the AMR of the SMC combining clusters from all regions. We try to explain the scenario to better understand the SMC chemo-dynamical history. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.08709v1-abstract-full').style.display = 'none'; document.getElementById('2307.08709v1-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 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 8 figures, 3 tables, Accepted for publication in Astronomy & Astrophysics journals</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 677, A35 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.05690">arXiv:2307.05690</a> <span> [<a href="https://arxiv.org/pdf/2307.05690">pdf</a>, <a href="https://arxiv.org/format/2307.05690">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"> Ages, metallicities and structure of stellar clusters in the Magellanic Bridge </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Oliveira%2C+R+A+P">Raphael A. P. Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Maia%2C+F+F+S">Francisco F. S. Maia</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">Beatriz Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=Dias%2C+B">Bruno Dias</a>, <a href="/search/astro-ph?searchtype=author&query=collaboration%2C+t+V">the VISCACHA collaboration</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2307.05690v1-abstract-short" style="display: inline;"> The formation of the Magellanic Bridge during an encounter between the Magellanic Clouds $\sim$200 Myr ago would be imprinted in the chemical evolution and kinematics of its stellar population, with sites of active star formation. Since it contains hundreds of stellar clusters and associations, we combined deep photometry from VISCACHA and SMASH surveys to explore this topic, by deriving structura… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.05690v1-abstract-full').style.display = 'inline'; document.getElementById('2307.05690v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.05690v1-abstract-full" style="display: none;"> The formation of the Magellanic Bridge during an encounter between the Magellanic Clouds $\sim$200 Myr ago would be imprinted in the chemical evolution and kinematics of its stellar population, with sites of active star formation. Since it contains hundreds of stellar clusters and associations, we combined deep photometry from VISCACHA and SMASH surveys to explore this topic, by deriving structural parameters, age, metallicity, distance and mass for 33 Bridge clusters with robust statistical tools. We identified a group of 13 clusters probably stripped from the Small Magellanic Cloud (0.5$-$6.8 Gyr, $\rm{[Fe/H]} < -0.6$ dex) and another 15 probably formed in-situ ($<$200 Myr, $\rm{[Fe/H]}\sim-0.4$ dex). Two metallicity dips were detected in the age-metallicity relation, coeval to the Stream and Bridge formation epochs. Cluster masses range from 500 to $\sim 10^4 M_\odot$, and a new estimate of $3-5\times 10^5 M_\odot$ is obtained for the Bridge stellar mass. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.05690v1-abstract-full').style.display = 'none'; document.getElementById('2307.05690v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">4 pages, 3 figures, to appear in the proceedings of the IAUS379 "Dynamical Masses of Local Group Galaxies"</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.17333">arXiv:2306.17333</a> <span> [<a href="https://arxiv.org/pdf/2306.17333">pdf</a>, <a href="https://arxiv.org/format/2306.17333">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> <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/10.1088/1538-3873/ace3f7">10.1088/1538-3873/ace3f7 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Rubin Observatory LSST Stars Milky Way and Local Volume Star Clusters Roadmap </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Usher%2C+C">Christopher Usher</a>, <a href="/search/astro-ph?searchtype=author&query=Dage%2C+K+C">Kristen C. Dage</a>, <a href="/search/astro-ph?searchtype=author&query=Girardi%2C+L">L茅o Girardi</a>, <a href="/search/astro-ph?searchtype=author&query=Barmby%2C+P">Pauline Barmby</a>, <a href="/search/astro-ph?searchtype=author&query=Bonatto%2C+C+J">Charles J. Bonatto</a>, <a href="/search/astro-ph?searchtype=author&query=Chies-Santos%2C+A+L">Ana L. Chies-Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Clarkson%2C+W+I">William I. Clarkson</a>, <a href="/search/astro-ph?searchtype=author&query=Camus%2C+M+G">Matias G贸mez Camus</a>, <a href="/search/astro-ph?searchtype=author&query=Hartmann%2C+E+A">Eduardo A. Hartmann</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+A+M+N">Annette M. N. Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Pieres%2C+A">Adriano Pieres</a>, <a href="/search/astro-ph?searchtype=author&query=Prisinzano%2C+L">Loredana Prisinzano</a>, <a href="/search/astro-ph?searchtype=author&query=Rhode%2C+K+L">Katherine L. Rhode</a>, <a href="/search/astro-ph?searchtype=author&query=Rich%2C+R+M">R. Michael Rich</a>, <a href="/search/astro-ph?searchtype=author&query=Ripepi%2C+V">Vincenzo Ripepi</a>, <a href="/search/astro-ph?searchtype=author&query=Santiago%2C+B">Basilio Santiago</a>, <a href="/search/astro-ph?searchtype=author&query=Stassun%2C+K+G">Keivan G. Stassun</a>, <a href="/search/astro-ph?searchtype=author&query=Street%2C+R+A">R. A. Street</a>, <a href="/search/astro-ph?searchtype=author&query=Szab%C3%B3%2C+R">R贸bert Szab贸</a>, <a href="/search/astro-ph?searchtype=author&query=Venuti%2C+L">Laura Venuti</a>, <a href="/search/astro-ph?searchtype=author&query=Zaggia%2C+S">Simone Zaggia</a>, <a href="/search/astro-ph?searchtype=author&query=Canossa%2C+M">Marco Canossa</a>, <a href="/search/astro-ph?searchtype=author&query=Floriano%2C+P">Pedro Floriano</a>, <a href="/search/astro-ph?searchtype=author&query=Lopes%2C+P">Pedro Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Miranda%2C+N+L">Nicole L. Miranda</a> , et al. (4 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.17333v1-abstract-short" style="display: inline;"> The Vera C. Rubin Observatory will undertake the Legacy Survey of Space and Time, providing an unprecedented, volume-limited catalog of star clusters in the Southern Sky, including Galactic and extragalactic star clusters. The Star Clusters subgroup of the Stars, Milky Way and Local Volume Working Group has identified key areas where Rubin Observatory will enable significant progress in star clust… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.17333v1-abstract-full').style.display = 'inline'; document.getElementById('2306.17333v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.17333v1-abstract-full" style="display: none;"> The Vera C. Rubin Observatory will undertake the Legacy Survey of Space and Time, providing an unprecedented, volume-limited catalog of star clusters in the Southern Sky, including Galactic and extragalactic star clusters. The Star Clusters subgroup of the Stars, Milky Way and Local Volume Working Group has identified key areas where Rubin Observatory will enable significant progress in star cluster research. This roadmap represents our science cases and preparation for studies of all kinds of star clusters from the Milky Way out to distances of tens of megaparsecs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.17333v1-abstract-full').style.display = 'none'; document.getElementById('2306.17333v1-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 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">accepted to PASP</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.05503">arXiv:2306.05503</a> <span> [<a href="https://arxiv.org/pdf/2306.05503">pdf</a>, <a href="https://arxiv.org/format/2306.05503">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/stad1827">10.1093/mnras/stad1827 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The VISCACHA survey -- VII. Assembly history of the Magellanic Bridge and SMC Wing from star clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Oliveira%2C+R+A+P">R. A. P. Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Maia%2C+F+F+S">F. F. S. Maia</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">B. Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=Dias%2C+B">B. Dias</a>, <a href="/search/astro-ph?searchtype=author&query=Santos%2C+J+F+C">J. F. C. Santos Jr.</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=Kerber%2C+L+O">L. O. Kerber</a>, <a href="/search/astro-ph?searchtype=author&query=Bica%2C+E">E. Bica</a>, <a href="/search/astro-ph?searchtype=author&query=Sanmartim%2C+D">D. Sanmartim</a>, <a href="/search/astro-ph?searchtype=author&query=Quint%2C+B">B. Quint</a>, <a href="/search/astro-ph?searchtype=author&query=Fraga%2C+L">L. Fraga</a>, <a href="/search/astro-ph?searchtype=author&query=Armond%2C+T">T. Armond</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Parisi%2C+M+C">M. C. Parisi</a>, <a href="/search/astro-ph?searchtype=author&query=Santrich%2C+O+J+K">O. J. Katime Santrich</a>, <a href="/search/astro-ph?searchtype=author&query=Angelo%2C+M+S">M. S. Angelo</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A9rez-Villegas%2C+A">A. P茅rez-Villegas</a>, <a href="/search/astro-ph?searchtype=author&query=De+B%C3%B3rtoli%2C+B+J">B. J. De B贸rtoli</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="2306.05503v1-abstract-short" style="display: inline;"> The formation scenario of the Magellanic Bridge during an encounter between the Large and Small Magellanic Clouds $\sim200\,$Myr ago, as proposed by $N$-body models, would be imprinted in the chemical enrichment and kinematics of its stars, and sites of ongoing star formation along its extension. We present an analysis of 33 Bridge star clusters using photometry obtained with the SOAR 4-m telescop… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.05503v1-abstract-full').style.display = 'inline'; document.getElementById('2306.05503v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.05503v1-abstract-full" style="display: none;"> The formation scenario of the Magellanic Bridge during an encounter between the Large and Small Magellanic Clouds $\sim200\,$Myr ago, as proposed by $N$-body models, would be imprinted in the chemical enrichment and kinematics of its stars, and sites of ongoing star formation along its extension. We present an analysis of 33 Bridge star clusters using photometry obtained with the SOAR 4-m telescope equipped with adaptive optics for the VISCACHA survey. We performed a membership selection and derived self-consistent ages, metallicities, distances and reddening values via statistical isochrone fitting, as well as tidal radii and integrated masses from structure analysis. Two groups are clearly detected: 13 well-studied clusters older than the Bridge, with $0.5-6.8\,$Gyr and $\rm{[Fe/H]}<-0.6\,$dex; and 15 clusters with $< 200\,$Myr and $\rm{[Fe/H]}>-0.5\,$dex, probably formed in-situ. The old clusters follow the overall age and metallicity gradients of the SMC, whereas the younger ones are uniformly distributed along the Bridge. The main results are as follows: $(i)$ we derive ages and metallicities for the first time for 9 and 18 clusters, respectively; $(ii)$ we detect two metallicity dips in the age-metallicity relation of the Bridge at $\sim 200\,$Myr and $1.5\,$Gyr ago for the first time, possibly chemical signatures of the formation of the Bridge and Magellanic Stream; $(iii)$ we estimate a minimum stellar mass for the Bridge of $3-5 \times 10^5\,M_\odot$; $(iv)$ we confirm that all the young Bridge clusters at $\rm{RA} < 3^h$ are metal-rich $\rm{[Fe/H]} \sim -0.4\,$dex. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.05503v1-abstract-full').style.display = 'none'; document.getElementById('2306.05503v1-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 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">15 pages, 13 figures + appendix. 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/2212.09685">arXiv:2212.09685</a> <span> [<a href="https://arxiv.org/pdf/2212.09685">pdf</a>, <a href="https://arxiv.org/format/2212.09685">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> The VISCACHA survey -- VI. Dimensional study of the structure of 82 star clusters in the Magellanic Clouds </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rodr%C3%ADguez%2C+M+J">M. Jimena Rodr铆guez</a>, <a href="/search/astro-ph?searchtype=author&query=Feinstein%2C+C">C. Feinstein</a>, <a href="/search/astro-ph?searchtype=author&query=Baume%2C+G">G. Baume</a>, <a href="/search/astro-ph?searchtype=author&query=Dias%2C+B">B. Dias</a>, <a href="/search/astro-ph?searchtype=author&query=Maia%2C+F+S+M">F. S. M. Maia</a>, <a href="/search/astro-ph?searchtype=author&query=Santos%2C+J+F+C">J. F. C. Santos Jr.</a>, <a href="/search/astro-ph?searchtype=author&query=Kerber%2C+L">L. Kerber</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A9rez-Villegas%2C+A">A. P茅rez-Villegas</a>, <a href="/search/astro-ph?searchtype=author&query=De+B%C3%B3rtoli%2C+B">B. De B贸rtoli</a>, <a href="/search/astro-ph?searchtype=author&query=Parisi%2C+M+C">M. C. Parisi</a>, <a href="/search/astro-ph?searchtype=author&query=Oliveira%2C+R+A+P">R. A. P. Oliveira</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2212.09685v1-abstract-short" style="display: inline;"> We present a study of the internal structure of 82 star clusters located at the outer regions of the Large Magellanic Cloud and the Small Magellanic Cloud using data of the VISCACHA Survey. Through the construction of the minimum spanning tree, which analyzes the relative position of stars within a given cluster, it was possible to characterize the internal structure and explore the fractal or sub… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.09685v1-abstract-full').style.display = 'inline'; document.getElementById('2212.09685v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.09685v1-abstract-full" style="display: none;"> We present a study of the internal structure of 82 star clusters located at the outer regions of the Large Magellanic Cloud and the Small Magellanic Cloud using data of the VISCACHA Survey. Through the construction of the minimum spanning tree, which analyzes the relative position of stars within a given cluster, it was possible to characterize the internal structure and explore the fractal or subclustered distribution for each cluster. We computed the parameters m (which is the average length of the connected segments normalized by the area), s (which is the mean points separation in units of cluster radius), and Q (the ratio of these components). These parameters are useful to distinguish between radial, homogeneous, and substructured distributions of stars. The dependence of these parameters with the different characteristics of the clusters, such as their ages and spatial distribution, was also studied. We found that most of the studied clusters present a homogeneous stellar distribution or a distribution with a radial concentration. Our results are consistent with the models, suggesting that more dynamically evolved clusters seem to have larger Q values, confirming previous results from numerical simulations. There also seems to be a correlation between the internal structure of the clusters and their galactocentric distances, in the sense that for both galaxies, the more distant clusters have larger Q values. We also paid particular attention to the effects of contamination by non-member field stars and its consequences finding that field star decontamination is crucial for these kinds of studies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.09685v1-abstract-full').style.display = 'none'; document.getElementById('2212.09685v1-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 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">9 pages, 11 figures, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.05532">arXiv:2209.05532</a> <span> [<a href="https://arxiv.org/pdf/2209.05532">pdf</a>, <a href="https://arxiv.org/format/2209.05532">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/slac108">10.1093/mnrasl/slac108 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The VISCACHA survey -- V. Rejuvenating three faint SMC clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bica%2C+E">E. Bica</a>, <a href="/search/astro-ph?searchtype=author&query=Maia%2C+F+F+S">F. F. S. Maia</a>, <a href="/search/astro-ph?searchtype=author&query=Oliveira%2C+R+A+P">R. A. P. Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Dias%2C+B">B. Dias</a>, <a href="/search/astro-ph?searchtype=author&query=Santos%2C+J+F+C">J. F. C. Santos Jr.</a>, <a href="/search/astro-ph?searchtype=author&query=Rocha%2C+J+P">J. P. Rocha</a>, <a href="/search/astro-ph?searchtype=author&query=Kerber%2C+L">L. Kerber</a>, <a href="/search/astro-ph?searchtype=author&query=Gardin%2C+J+F">J. F. Gardin</a>, <a href="/search/astro-ph?searchtype=author&query=Armond%2C+T">T. Armond</a>, <a href="/search/astro-ph?searchtype=author&query=Parisi%2C+M+C">M. C. Parisi</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=Barbuy%2C+B">B. Barbuy</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="2209.05532v1-abstract-short" style="display: inline;"> We present the analysis of three faint clusters of the Small Magellanic Cloud RZ82, HW42 and RZ158. We employed the SOAR telescope instrument SAM with adaptive optics, allowing us to reach to V~23-24 mag, unprecedentedly, a depth sufficient to measure ages of up to about 10-12Gyr. All three clusters are resolved to their centres, and the resulting colour-magnitude diagrams (CMDs) allow us to deriv… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.05532v1-abstract-full').style.display = 'inline'; document.getElementById('2209.05532v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.05532v1-abstract-full" style="display: none;"> We present the analysis of three faint clusters of the Small Magellanic Cloud RZ82, HW42 and RZ158. We employed the SOAR telescope instrument SAM with adaptive optics, allowing us to reach to V~23-24 mag, unprecedentedly, a depth sufficient to measure ages of up to about 10-12Gyr. All three clusters are resolved to their centres, and the resulting colour-magnitude diagrams (CMDs) allow us to derive ages of 3.9, 2.6, and 4.8Gyr respectively. These results are significantly younger than previous determinations (7.1, 5.0, and 8.3Gyr, respectively), based on integrated photometry or shallower CMDs. We rule out older ages for these clusters based on deep photometry and statistical isochrone fitting. We also estimate metallicities for the three clusters of [Fe/H]=-0.68, -0.57 and -0.90, respectively. These updated ages and metallicities are in good agreement with the age-metallicity relation for the bulk of SMC clusters. Total cluster masses ranging from ~7-11x10^3Mo were estimated from integrated flux, consistent with masses estimated for other SMC clusters of similar ages. These results reduce the number of SMC clusters known to be older than about 5 Gyr and highlight the need of deep and spatially resolved photometry to determine accurate ages for older, low-luminosity SMC star clusters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.05532v1-abstract-full').style.display = 'none'; document.getElementById('2209.05532v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication as MNRAS letter, 5 pages, 5 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.11119">arXiv:2201.11119</a> <span> [<a href="https://arxiv.org/pdf/2201.11119">pdf</a>, <a href="https://arxiv.org/ps/2201.11119">ps</a>, <a href="https://arxiv.org/format/2201.11119">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/stac259">10.1093/mnras/stac259 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The VISCACHA survey -- IV. The SMC West Halo in 8D </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dias%2C+B">B. Dias</a>, <a href="/search/astro-ph?searchtype=author&query=Parisi%2C+M+C">M. C. Parisi</a>, <a href="/search/astro-ph?searchtype=author&query=Angelo%2C+M">M. Angelo</a>, <a href="/search/astro-ph?searchtype=author&query=Maia%2C+F">F. Maia</a>, <a href="/search/astro-ph?searchtype=author&query=Oliveira%2C+R+A+P">R. A. P. Oliveira</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=Kerber%2C+L+O">L. O. Kerber</a>, <a href="/search/astro-ph?searchtype=author&query=Santos%2C+J+F+C">J. F. C. Santos Jr.</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A9rez-Villegas%2C+A">A. P茅rez-Villegas</a>, <a href="/search/astro-ph?searchtype=author&query=Sanmartim%2C+D">D. Sanmartim</a>, <a href="/search/astro-ph?searchtype=author&query=Quint%2C+B">B. Quint</a>, <a href="/search/astro-ph?searchtype=author&query=Fraga%2C+L">L. Fraga</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">B. Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=Bica%2C+E">E. Bica</a>, <a href="/search/astro-ph?searchtype=author&query=Santrich%2C+O+J+K">O. J. Katime Santrich</a>, <a href="/search/astro-ph?searchtype=author&query=Hernandez-Jimenez%2C+J+A">J. A. Hernandez-Jimenez</a>, <a href="/search/astro-ph?searchtype=author&query=Geisler%2C+D">D. Geisler</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=De+B%C3%B3rtoli%2C+B+J">B. J. De B贸rtoli</a>, <a href="/search/astro-ph?searchtype=author&query=Bassino%2C+L+P">L. P. Bassino</a>, <a href="/search/astro-ph?searchtype=author&query=Rocha%2C+J+P">J. P. Rocha</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="2201.11119v1-abstract-short" style="display: inline;"> The structure of the Small Magellanic Cloud (SMC) is very complex, in particular in the periphery that suffers more from the interactions with the Large Magellanic Cloud (LMC). A wealth of observational evidence has been accumulated revealing tidal tails and bridges made up of gas, stars and star clusters. Nevertheless, a full picture of the SMC outskirts is only recently starting to emerge with a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.11119v1-abstract-full').style.display = 'inline'; document.getElementById('2201.11119v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.11119v1-abstract-full" style="display: none;"> The structure of the Small Magellanic Cloud (SMC) is very complex, in particular in the periphery that suffers more from the interactions with the Large Magellanic Cloud (LMC). A wealth of observational evidence has been accumulated revealing tidal tails and bridges made up of gas, stars and star clusters. Nevertheless, a full picture of the SMC outskirts is only recently starting to emerge with a 6D phase-space map plus age and metallicity using star clusters as tracers. In this work, we continue our analysis of another outer region of the SMC, the so-called West Halo, and combined it with the previously analysed Northern Bridge. We use both structures to define the Bridge and Counter-bridge trailing and leading tidal tails. These two structures are moving away from each other, roughly in the SMC-LMC direction. The West Halo form a ring around the SMC inner regions that goes up to the background of the Northern Bridge shaping an extended layer of the Counter-bridge. Four old Bridge clusters were identified at distances larger than 8 kpc from the SMC centre moving towards the LMC, which is consistent with the SMC-LMC closest distance of 7.5 kpc when the Magellanic Bridge was formed about 150Myr ago; this shows that the Magellanic Bridge was not formed only by pulled gas, but it also removed older stars from the SMC during its formation. We also found age and metallicity radial gradients using projected distances on sky, which are vanished when we use the real 3D distances. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.11119v1-abstract-full').style.display = 'none'; document.getElementById('2201.11119v1-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, 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">14 pages, 8 figures + appendix. 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/2110.13943">arXiv:2110.13943</a> <span> [<a href="https://arxiv.org/pdf/2110.13943">pdf</a>, <a href="https://arxiv.org/format/2110.13943">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/10.1051/0004-6361/202141596">10.1051/0004-6361/202141596 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Precise distances from OGLE-IV member RR Lyrae stars in six bulge globular clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Oliveira%2C+R+A+P">R. A. P. Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Ortolani%2C+S">S. Ortolani</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">B. Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=Kerber%2C+L+O">L. O. Kerber</a>, <a href="/search/astro-ph?searchtype=author&query=Maia%2C+F+F+S">F. F. S. Maia</a>, <a href="/search/astro-ph?searchtype=author&query=Bica%2C+E">E. Bica</a>, <a href="/search/astro-ph?searchtype=author&query=Cassisi%2C+S">S. Cassisi</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=P%C3%A9rez-Villegas%2C+A">A. P茅rez-Villegas</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2110.13943v1-abstract-short" style="display: inline;"> Context. RR Lyrae stars are useful standard candles allowing one to derive accurate distances for old star clusters. Based on the recent catalogues from OGLE-IV and Gaia Early Data Release 3 (EDR3), the distances can be improved for a few bulge globular clusters. Aims. The aim of this work is to derive an accurate distance for the following six moderately metal-poor, relatively high-reddening bulg… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.13943v1-abstract-full').style.display = 'inline'; document.getElementById('2110.13943v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.13943v1-abstract-full" style="display: none;"> Context. RR Lyrae stars are useful standard candles allowing one to derive accurate distances for old star clusters. Based on the recent catalogues from OGLE-IV and Gaia Early Data Release 3 (EDR3), the distances can be improved for a few bulge globular clusters. Aims. The aim of this work is to derive an accurate distance for the following six moderately metal-poor, relatively high-reddening bulge globular clusters: NGC 6266, NGC 6441, NGC 6626, NGC 6638, NGC 6642, and NGC 6717. Methods. We combined newly available OGLE-IV catalogues of variable stars containing mean I magnitudes, with Clement's previous catalogues containing mean V magnitudes, and with precise proper motions from Gaia EDR3. Astrometric membership probabilities were computed for each RR Lyrae, in order to select those compatible with the cluster proper motions. Applying luminosity-metallicity relations derived from BaSTI $伪$-enhanced models (He-enhanced for NGC 6441 and canonical He for the other clusters), we updated the distances with relatively low uncertainties. Results. Distances were derived with the I and V bands, with a $5-8\%$ precision. We obtained 6.6 kpc, 13.1 kpc, 5.6 kpc, 9.6 kpc, 8.2 kpc, and 7.3 kpc for NGC 6266, NGC 6441, NGC 6626, NGC 6638, NGC 6642, and NGC 6717, respectively. The results are in excellent agreement with the literature for all sample clusters, considering the uncertainties. Conclusions. The present method of distance derivation, based on recent data of member RR Lyrae stars, updated BaSTI models, and robust statistical methods, proved to be consistent. A larger sample of clusters will be investigated in a future work. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.13943v1-abstract-full').style.display = 'none'; document.getElementById('2110.13943v1-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 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 7 figures. Accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 657, A123 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2103.02600">arXiv:2103.02600</a> <span> [<a href="https://arxiv.org/pdf/2103.02600">pdf</a>, <a href="https://arxiv.org/format/2103.02600">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/10.1051/0004-6361/202040015">10.1051/0004-6361/202040015 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The VISCACHA survey -- III. Star clusters counterpart of the Magellanic Bridge and Counter-Bridge in 8D </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dias%2C+B">B. Dias</a>, <a href="/search/astro-ph?searchtype=author&query=Angelo%2C+M+S">M. S. Angelo</a>, <a href="/search/astro-ph?searchtype=author&query=Oliveira%2C+R+A+P">R. A. P. Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Maia%2C+F">F. Maia</a>, <a href="/search/astro-ph?searchtype=author&query=Parisi%2C+M+C">M. C. Parisi</a>, <a href="/search/astro-ph?searchtype=author&query=De+Bortoli%2C+B">B. De Bortoli</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=Santrich%2C+O+J+K">O. J. Katime Santrich</a>, <a href="/search/astro-ph?searchtype=author&query=Bassino%2C+L+P">L. P. Bassino</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">B. Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=Bica%2C+E">E. Bica</a>, <a href="/search/astro-ph?searchtype=author&query=Geisler%2C+D">D. Geisler</a>, <a href="/search/astro-ph?searchtype=author&query=Kerber%2C+L">L. Kerber</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A9rez-Villegas%2C+A">A. P茅rez-Villegas</a>, <a href="/search/astro-ph?searchtype=author&query=Quint%2C+B">B. Quint</a>, <a href="/search/astro-ph?searchtype=author&query=Sanmartim%2C+D">D. Sanmartim</a>, <a href="/search/astro-ph?searchtype=author&query=Santos%2C+J+F+C">J. F. C. Santos Jr.</a>, <a href="/search/astro-ph?searchtype=author&query=Westera%2C+P">P. Westera</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2103.02600v1-abstract-short" style="display: inline;"> Context. The interactions between the SMC and LMC created the Magellanic Bridge, a stream of gas and stars pulled out of the SMC towards the LMC about 150 Myr ago. The tidal counterpart of this structure, which should include a trailing arm, has been predicted by models but no compelling observational evidence has confirmed the Counter-Bridge so far. Aims. The main goal of this work is to find the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.02600v1-abstract-full').style.display = 'inline'; document.getElementById('2103.02600v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.02600v1-abstract-full" style="display: none;"> Context. The interactions between the SMC and LMC created the Magellanic Bridge, a stream of gas and stars pulled out of the SMC towards the LMC about 150 Myr ago. The tidal counterpart of this structure, which should include a trailing arm, has been predicted by models but no compelling observational evidence has confirmed the Counter-Bridge so far. Aims. The main goal of this work is to find the stellar counterpart of the Magellanic Bridge and Counter-Bridge. We use star clusters in the SMC outskirts as they provide 6D phase-space vector, age and metallicity that help characterise the outskirts of the SMC. Methods. Distances, ages and photometric metallicities are derived from fitting isochrones to the colour-magnitude diagrams from the VISCACHA survey. Radial velocities and spectroscopic metallicities are derived from the spectroscopic follow-up using GMOS in the CaII triplet region. Results. Among the seven clusters analysed in this work, five belong to the Magellanic Bridge and one belongs to the Counter-Bridge and the other to the transition region. Conclusions. The existence of the tidal counterpart of the Magellanic Bridge is evidenced by star clusters. The stellar component of the Magellanic Bridge and Counter-Bridge are confirmed in the SMC outskirts. These results are an important constraint for models that seek to reconstruct the history of the orbit and interactions between LMC-SMC and constrain their future interaction including with the Milky Way. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.02600v1-abstract-full').style.display = 'none'; document.getElementById('2103.02600v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 7 figures. Astronomy and Astrophysics Letter, accepted. For associated video file (fig.A.4), see https://drive.google.com/file/d/1mSx3z6vDjHUneEeVq1i-MHwXZ1O0pZ-f</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 647, L9 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2001.08611">arXiv:2001.08611</a> <span> [<a href="https://arxiv.org/pdf/2001.08611">pdf</a>, <a href="https://arxiv.org/format/2001.08611">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/ab6f76">10.3847/1538-4357/ab6f76 <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. XX. Ages of single and multiple stellar populations in seven bulge globular clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Oliveira%2C+R+A+P">R. A. P. Oliveira</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=Kerber%2C+L+O">L. O. Kerber</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">B. Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=Ortolani%2C+S">S. Ortolani</a>, <a href="/search/astro-ph?searchtype=author&query=Piotto%2C+G">G. Piotto</a>, <a href="/search/astro-ph?searchtype=author&query=Nardiello%2C+D">D. Nardiello</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A9rez-Villegas%2C+A">A. P茅rez-Villegas</a>, <a href="/search/astro-ph?searchtype=author&query=Maia%2C+F+F+S">F. F. S. Maia</a>, <a href="/search/astro-ph?searchtype=author&query=Bica%2C+E">E. Bica</a>, <a href="/search/astro-ph?searchtype=author&query=Cassisi%2C+S">S. Cassisi</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=Lagioia%2C+E">E. Lagioia</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=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=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=King%2C+I+R">I. R. King</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=Pietrinferni%2C+A">A. Pietrinferni</a>, <a href="/search/astro-ph?searchtype=author&query=Renzini%2C+A">A. Renzini</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">A. Sarajedini</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Marel%2C+R">R. van der Marel</a> , et al. (1 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2001.08611v1-abstract-short" style="display: inline;"> In the present work we analyzed seven globular clusters selected from their location in the Galactic bulge and with metallicity values in the range $-1.30\lesssim\rm{[Fe/H]}\lesssim-0.50$. The aim of this work is first to derive cluster ages assuming single stellar populations, and secondly, to identify the stars from first (1G) and second generations (2G) from the main sequence, subgiant and red… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.08611v1-abstract-full').style.display = 'inline'; document.getElementById('2001.08611v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2001.08611v1-abstract-full" style="display: none;"> In the present work we analyzed seven globular clusters selected from their location in the Galactic bulge and with metallicity values in the range $-1.30\lesssim\rm{[Fe/H]}\lesssim-0.50$. The aim of this work is first to derive cluster ages assuming single stellar populations, and secondly, to identify the stars from first (1G) and second generations (2G) from the main sequence, subgiant and red giant branches, and to derive their age differences. Based on a combination of UV and optical filters used in this project, we apply the Gaussian mixture models to distinguish the multiple stellar populations. Applying statistical isochrone fitting, we derive self-consistent ages, distances, metallicities, and reddening values for the sample clusters. An average of $12.3\pm0.4$ Gyr was obtained both using Dartmouth and BaSTI (accounting atomic diffusion effects) isochrones, without a clear distinction between the moderately metal-poor and the more metal-rich bulge clusters, except for NGC 6717 and the inner halo NGC 6362 with $\sim 13.5$ Gyr. We derived a weighted mean age difference between the multiple populations hosted by each globular cluster of $41\pm170$ Myr adopting canonical He abundances; whereas for higher He in 2G stars, this difference reduces to $17\pm170$ Myr, but with individual uncertainties of $500$ Myr. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.08611v1-abstract-full').style.display = 'none'; document.getElementById('2001.08611v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 16 figures and 7 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/2001.02697">arXiv:2001.02697</a> <span> [<a href="https://arxiv.org/pdf/2001.02697">pdf</a>, <a href="https://arxiv.org/format/2001.02697">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/ab6a0f">10.3847/1538-4357/ab6a0f <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Self-consistent analysis of stellar clusters: An application to HST data of the halo globular cluster NGC 6752 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Souza%2C+S+O">Stefano O. Souza</a>, <a href="/search/astro-ph?searchtype=author&query=Kerber%2C+L+O">Leandro O. Kerber</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">Beatriz Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A9rez-Villegas%2C+A">Angeles P茅rez-Villegas</a>, <a href="/search/astro-ph?searchtype=author&query=Oliveira%2C+R+A+P">Raphael A. P. Oliveira</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="2001.02697v1-abstract-short" style="display: inline;"> The Bayesian isochrone fitting using the Markov chain Monte Carlo algorithm is applied, to derive the probability distribution of the parameters age, metallicity, reddening, and absolute distance modulus. We introduce the \texttt{SIRIUS} code by means of simulated color-magnitude diagrams, including the analysis of multiple stellar populations. The population tagging is applied from the red giant… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.02697v1-abstract-full').style.display = 'inline'; document.getElementById('2001.02697v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2001.02697v1-abstract-full" style="display: none;"> The Bayesian isochrone fitting using the Markov chain Monte Carlo algorithm is applied, to derive the probability distribution of the parameters age, metallicity, reddening, and absolute distance modulus. We introduce the \texttt{SIRIUS} code by means of simulated color-magnitude diagrams, including the analysis of multiple stellar populations. The population tagging is applied from the red giant branch to the bottom of the main sequence. Through sanity checks using synthetic {\it HST} color-magnitude diagrams of globular clusters we verify the code reliability in the context of simple and multiple stellar populations. In such tests, the formal uncertainties in age or age difference, metallicity, reddening, and absolute distance modulus can reach $400$ Myr, $0.03$ dex, $0.01$ mag, and $0.03$ mag, respectively. We apply the method to analyse NGC 6752, using Dartmouth stellar evolutionary models. Assuming a single stellar population, we derive an age of $13.7\pm0.5$ Gyr and a distance of $d_{\odot}=4.11\pm 0.08$ kpc, with the latter in agreement within $~3蟽$ with the inverse Gaia parallax. In the analysis of the multiple stellar populations, three {populations} are clearly identified. From the Chromosome Map and UV/Optical two-color diagrams inspection, we found a fraction of stars of $25\pm5$, $46\pm7$, and $29\pm5$ per cent, for the first, second, and third generations, respectively. These fractions are in good agreement with the literature. An age difference of $500\pm410$ Myr between the first and the third generation is found, with the uncertainty decreasing to $400$ Myr when the helium enhancement is taken into account. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.02697v1-abstract-full').style.display = 'none'; document.getElementById('2001.02697v1-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 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 11 figures, 3 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/1909.02566">arXiv:1909.02566</a> <span> [<a href="https://arxiv.org/pdf/1909.02566">pdf</a>, <a href="https://arxiv.org/format/1909.02566">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/10.1017/S174392131900694X">10.1017/S174392131900694X <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The VISCACHA survey -- deep and resolved photometry of star clusters in the Magellanic Clouds </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dias%2C+B">Bruno Dias</a>, <a href="/search/astro-ph?searchtype=author&query=Maia%2C+F">Francisco Maia</a>, <a href="/search/astro-ph?searchtype=author&query=Kerber%2C+L">Leandro Kerber</a>, <a href="/search/astro-ph?searchtype=author&query=Santos%2C+J+F+C+d">Jo茫o F. C. dos Santos Jr.</a>, <a href="/search/astro-ph?searchtype=author&query=Bica%2C+E">Eduardo Bica</a>, <a href="/search/astro-ph?searchtype=author&query=Armond%2C+T">Tina Armond</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">Beatriz Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=Fraga%2C+L">Luciano Fraga</a>, <a href="/search/astro-ph?searchtype=author&query=Hernandez-Jimenez%2C+J+A">Jose A. Hernandez-Jimenez</a>, <a href="/search/astro-ph?searchtype=author&query=Santrich%2C+O+J+K">Orlando J. Katime Santrich</a>, <a href="/search/astro-ph?searchtype=author&query=Oliveira%2C+R+A+P">Raphael A. P. Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A9rez-Villegas%2C+A">Angeles P茅rez-Villegas</a>, <a href="/search/astro-ph?searchtype=author&query=Piatti%2C+A">Andres Piatti</a>, <a href="/search/astro-ph?searchtype=author&query=Quint%2C+B">Bruno Quint</a>, <a href="/search/astro-ph?searchtype=author&query=Sanmartin%2C+D">David Sanmartin</a>, <a href="/search/astro-ph?searchtype=author&query=Angelo%2C+M+S">Mateus S. Angelo</a>, <a href="/search/astro-ph?searchtype=author&query=Souza%2C+S+O">Stefano O. Souza</a>, <a href="/search/astro-ph?searchtype=author&query=Vieira%2C+R+G">Rodrigo G. Vieira</a>, <a href="/search/astro-ph?searchtype=author&query=Westera%2C+P">Pieter Westera</a>, <a href="/search/astro-ph?searchtype=author&query=Parisi%2C+C">Celeste Parisi</a>, <a href="/search/astro-ph?searchtype=author&query=Geisler%2C+D">Doug Geisler</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">Dante Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Saito%2C+R">Roberto Saito</a>, <a href="/search/astro-ph?searchtype=author&query=Bassino%2C+L">Lilia Bassino</a>, <a href="/search/astro-ph?searchtype=author&query=De+Bortoli%2C+B">Bruno De Bortoli</a> , et al. (2 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1909.02566v1-abstract-short" style="display: inline;"> The VISCACHA (VIsible Soar photometry of star Clusters in tApii and Coxi HuguA\footnote{LMC and SMC names in the Tupi-Guarani language spoken by native people in Brazil}) Survey is an ongoing project based on deep and spatiallyresolved photometric observations of Magellanic Cloud star clusters, collected using the SOuthern Astrophysical Research (SOAR) telescope together with the SOAR Adaptive Mod… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.02566v1-abstract-full').style.display = 'inline'; document.getElementById('1909.02566v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1909.02566v1-abstract-full" style="display: none;"> The VISCACHA (VIsible Soar photometry of star Clusters in tApii and Coxi HuguA\footnote{LMC and SMC names in the Tupi-Guarani language spoken by native people in Brazil}) Survey is an ongoing project based on deep and spatiallyresolved photometric observations of Magellanic Cloud star clusters, collected using the SOuthern Astrophysical Research (SOAR) telescope together with the SOAR Adaptive Module Imager. So far we have used $>$300h of telescope time to observe $\sim$150 star clusters, mostly with low mass ($M < 10^4 M_{\odot}$) on the outskirts of the LMC and SMC. With this high-quality data set, we homogeneously determine physical properties using deep colour-magnitude diagrams (ages, metallicities, reddening, distances, mass, luminosity and mass functions) and structural parameters (radial density profiles, sizes) for these clusters which are used as a proxy to investigate the interplay between the Magellanic Clouds and their evolution. We present the VISCACHA survey and its initial results, based on our first two papers. The project's long term goals and expected legacy to the community are also addressed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.02566v1-abstract-full').style.display = 'none'; document.getElementById('1909.02566v1-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 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">4 pages, 2 figures, to appear in the proceedings of the IAUS351 "Star Clusters: From the Milky Way to the Early Universe", A. Bragaglia, M.B. Davies, A. Sills & E. Vesperini, eds</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> IAU-19-IAUS351-0212 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1907.08642">arXiv:1907.08642</a> <span> [<a href="https://arxiv.org/pdf/1907.08642">pdf</a>, <a href="https://arxiv.org/format/1907.08642">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/10.3847/1538-3881/ab6595">10.3847/1538-3881/ab6595 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An Updated SMC and Magellanic Bridge Catalog of Star Clusters, Associations and Related Objects </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bica%2C+E">Eduardo Bica</a>, <a href="/search/astro-ph?searchtype=author&query=Westera%2C+P">Pieter Westera</a>, <a href="/search/astro-ph?searchtype=author&query=Kerber%2C+L+d+O">Leandro de O. Kerber</a>, <a href="/search/astro-ph?searchtype=author&query=Dias%2C+B">Bruno Dias</a>, <a href="/search/astro-ph?searchtype=author&query=Maia%2C+F">Francisco Maia</a>, <a href="/search/astro-ph?searchtype=author&query=Santos%2C+J+F+C">Jo茫o F. C. Santos Jr.</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">Beatriz Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=Oliveira%2C+R+A+P">Raphael A. P. Oliveira</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="1907.08642v2-abstract-short" style="display: inline;"> We present a catalog of star clusters, associations and related extended objects in the Small Magellanic Cloud and the Magellanic Bridge with 2741 entries, a factor 2 more than a previous version from a decade ago. Literature data till December 2018 are included. The identification of star clusters was carried out with digital atlases in various bands currently available in DSS and MAMA imaging su… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1907.08642v2-abstract-full').style.display = 'inline'; document.getElementById('1907.08642v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1907.08642v2-abstract-full" style="display: none;"> We present a catalog of star clusters, associations and related extended objects in the Small Magellanic Cloud and the Magellanic Bridge with 2741 entries, a factor 2 more than a previous version from a decade ago. Literature data till December 2018 are included. The identification of star clusters was carried out with digital atlases in various bands currently available in DSS and MAMA imaging surveys. In particular, we cross-identified recent cluster samples from the VMC, OGLE-IV and SMASH surveys, confirming new clusters and pointing out equivalencies. A major contribution of the present catalog consists in the accurate central positions for clusters and small associations, including a new sample of 45 clusters or candidates in the SMC and 19 in the Bridge, as well as a compilation of the most reliable age and metallicity values from the literature. A general catalog must also deal with the recent discoveries of 27 faint and ultra-faint star clusters and galaxies projected on the far surroundings of the Clouds, most of them from the DES survey. The information on these objects has been complemented with photometric, spectroscopic and kinematical follow-up data from the literature. The underluminous galaxies around the Magellanic System, still very few as compared to the predictions from $螞$ Cold Dark Matter simulations, can bring constraints to galaxy formation and hierarchical evolution. Furthermore, we provide diagnostics, when possible, of the nature of the ultra-faint clusters, searching for borders of the Magellanic System extensions into the Milky Way gravitational potential. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1907.08642v2-abstract-full').style.display = 'none'; document.getElementById('1907.08642v2-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 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 July, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 13 figures and 4 tables. Updated to match accepted version in AJ. The updated catalog is provided in full as ancillary file</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1902.01959">arXiv:1902.01959</a> <span> [<a href="https://arxiv.org/pdf/1902.01959">pdf</a>, <a href="https://arxiv.org/ps/1902.01959">ps</a>, <a href="https://arxiv.org/format/1902.01959">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/stz369">10.1093/mnras/stz369 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The VISCACHA survey - I. Overview and First Results </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Maia%2C+F+F+S">Francisco F. S. Maia</a>, <a href="/search/astro-ph?searchtype=author&query=Dias%2C+B">Bruno Dias</a>, <a href="/search/astro-ph?searchtype=author&query=Santos%2C+J+F+C">Jo茫o F. C. Santos Jr.</a>, <a href="/search/astro-ph?searchtype=author&query=Kerber%2C+L+d+O">Leandro de O. Kerber</a>, <a href="/search/astro-ph?searchtype=author&query=Bica%2C+E">Eduardo Bica</a>, <a href="/search/astro-ph?searchtype=author&query=Piatti%2C+A+E">Andr茅s E. Piatti</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">Beatriz Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=Quint%2C+B">Bruno Quint</a>, <a href="/search/astro-ph?searchtype=author&query=Fraga%2C+L">Luciano Fraga</a>, <a href="/search/astro-ph?searchtype=author&query=Sanmartim%2C+D">David Sanmartim</a>, <a href="/search/astro-ph?searchtype=author&query=Angelo%2C+M+S">Mateus S. Angelo</a>, <a href="/search/astro-ph?searchtype=author&query=Hernandez-Jimenez%2C+J+A">Jose A. Hernandez-Jimenez</a>, <a href="/search/astro-ph?searchtype=author&query=Santrich%2C+O+J+K">Orlando J. Katime Santrich</a>, <a href="/search/astro-ph?searchtype=author&query=Oliveira%2C+R+A+P">Raphael A. P. Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A9rez-Villegas%2C+A">Angeles P茅rez-Villegas</a>, <a href="/search/astro-ph?searchtype=author&query=Souza%2C+S+O">Stefano O. Souza</a>, <a href="/search/astro-ph?searchtype=author&query=Vieira%2C+R+G">Rodrigo G. Vieira</a>, <a href="/search/astro-ph?searchtype=author&query=Westera%2C+P">Pieter Westera</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1902.01959v1-abstract-short" style="display: inline;"> The VISCACHA (VIsible Soar photometry of star Clusters in tApii and Coxi HuguA) Survey is an ongoing project based on deep photometric observations of Magellanic Cloud star clusters, collected using the SOuthern Astrophysical Research (SOAR) telescope together with the SOAR Adaptive Module Imager. Since 2015 more than 200 hours of telescope time were used to observe about 130 stellar clusters, mos… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.01959v1-abstract-full').style.display = 'inline'; document.getElementById('1902.01959v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1902.01959v1-abstract-full" style="display: none;"> The VISCACHA (VIsible Soar photometry of star Clusters in tApii and Coxi HuguA) Survey is an ongoing project based on deep photometric observations of Magellanic Cloud star clusters, collected using the SOuthern Astrophysical Research (SOAR) telescope together with the SOAR Adaptive Module Imager. Since 2015 more than 200 hours of telescope time were used to observe about 130 stellar clusters, most of them with low mass (M < 10$^4$ M$_\odot$) and/or located in the outermost regions of the Large Magellanic Cloud and the Small Magellanic Cloud. With this high quality data set, we homogeneously determine physical properties from statistical analysis of colour-magnitude diagrams, radial density profiles, luminosity functions and mass functions. Ages, metallicities, reddening, distances, present-day masses, mass function slopes and structural parameters for these clusters are derived and used as a proxy to investigate the interplay between the environment in the Magellanic Clouds and the evolution of such systems. In this first paper we present the VISCACHA Survey and its initial results, concerning the SMC clusters AM3, K37, HW20 and NGC796 and the LMC ones KMHK228, OHSC3, SL576, SL61 and SL897, chosen to compose a representative subset of our cluster sample. The project's long term goals and legacy to the community are also addressed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.01959v1-abstract-full').style.display = 'none'; document.getElementById('1902.01959v1-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 February, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 21 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/1901.03721">arXiv:1901.03721</a> <span> [<a href="https://arxiv.org/pdf/1901.03721">pdf</a>, <a href="https://arxiv.org/format/1901.03721">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/stz003">10.1093/mnras/stz003 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Deep View of a Fossil Relic in the Galactic Bulge: The Globular Cluster HP$\,$1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kerber%2C+L+O">L. O. Kerber</a>, <a href="/search/astro-ph?searchtype=author&query=Libralato%2C+M">M. Libralato</a>, <a href="/search/astro-ph?searchtype=author&query=Souza%2C+S+O">S. O. Souza</a>, <a href="/search/astro-ph?searchtype=author&query=Oliveira%2C+R+A+P">R. A. P. Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Ortolani%2C+S">S. Ortolani</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A9rez-Villegas%2C+A">A. P茅rez-Villegas</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">B. Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=Dias%2C+B">B. Dias</a>, <a href="/search/astro-ph?searchtype=author&query=Bica%2C+E">E. Bica</a>, <a href="/search/astro-ph?searchtype=author&query=Nardiello%2C+D">D. Nardiello</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1901.03721v1-abstract-short" style="display: inline;"> HP$\,$1 is an $伪$-enhanced and moderately metal-poor bulge globular cluster with a blue horizontal branch. These combined characteristics make it a probable relic of the early star formation in the innermost Galactic regions. Here we present a detailed analysis of a deep near-infrared (NIR) photometry of HP$\,$1 obtained with the NIR GSAOI+GeMS camera at the Gemini-South telescope. $J$ and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.03721v1-abstract-full').style.display = 'inline'; document.getElementById('1901.03721v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1901.03721v1-abstract-full" style="display: none;"> HP$\,$1 is an $伪$-enhanced and moderately metal-poor bulge globular cluster with a blue horizontal branch. These combined characteristics make it a probable relic of the early star formation in the innermost Galactic regions. Here we present a detailed analysis of a deep near-infrared (NIR) photometry of HP$\,$1 obtained with the NIR GSAOI+GeMS camera at the Gemini-South telescope. $J$ and $K_{\rm S}$ images were collected with an exquisite spatial resolution (FWHM $\sim 0.1$ arcsec), reaching stars at two magnitudes below the MSTO. We combine our GSAOI data with archival F606W-filter $HST$ ACS/WFC images to compute relative proper motions and select bona fide cluster members. Results from statistical isochrone fits in the NIR and optical-NIR colour-magnitude diagrams indicate an age of $12.8^{+0.9}_{-0.8}$ Gyr, confirming that HP$\,$1 is one of the oldest clusters in the Milky Way. The same fits also provide apparent distance moduli in the $K_{\rm S}$ and $V$ filters in very good agreement with the ones from 11 RR Lyrae stars. By subtracting the extinction in each filter, we recover a heliocentric distance of $6.59^{+0.17}_{-0.15}$ kpc. Furthermore, we refine the orbit of HP$\,$1 using this accurate distance and update and accurate radial velocities (from high resolution spectroscopy) and absolute proper motions (from Gaia DR2), reaching mean perigalactic and apogalactic distances of $\sim$0.12 and $\sim$3 kpc respectively. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.03721v1-abstract-full').style.display = 'none'; document.getElementById('1901.03721v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 January, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 22 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/1802.02104">arXiv:1802.02104</a> <span> [<a href="https://arxiv.org/pdf/1802.02104">pdf</a>, <a href="https://arxiv.org/ps/1802.02104">ps</a>, <a href="https://arxiv.org/format/1802.02104">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/sty254">10.1093/mnras/sty254 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Near-infrared study of new embedded clusters in the Carina complex </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Oliveira%2C+R+A+P">R. A. P. Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Bica%2C+E">E. Bica</a>, <a href="/search/astro-ph?searchtype=author&query=Bonatto%2C+C">C. Bonatto</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="1802.02104v1-abstract-short" style="display: inline;"> We analyse the nature of a sample of stellar overdensities that we found projected on the Carina complex. This study is based on 2MASS photometry and involves the photometry decontamination of field stars, elaboration of intrinsic colour-magnitude diagrams J$\times$(J-Ks), colour-colour diagrams (J-H)$\times$(H-Ks) and radial density profiles, in order to determine the structure and the main astro… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.02104v1-abstract-full').style.display = 'inline'; document.getElementById('1802.02104v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1802.02104v1-abstract-full" style="display: none;"> We analyse the nature of a sample of stellar overdensities that we found projected on the Carina complex. This study is based on 2MASS photometry and involves the photometry decontamination of field stars, elaboration of intrinsic colour-magnitude diagrams J$\times$(J-Ks), colour-colour diagrams (J-H)$\times$(H-Ks) and radial density profiles, in order to determine the structure and the main astrophysical parameters of the best candidates. The verification of an overdensity as an embedded cluster requires a CMD consistent with a PMS content and MS stars, if any. From these results, we are able to verify if they are, in fact, embedded clusters. The results were, in general, rewarding: in a sample of 101 overdensities, the analysis provided 15 candidates, of which three were previously catalogued as clusters (CCCP-Cl$\,$16, Treasure Chest and FSR$\,$1555), and the 12 remaining are discoveries that provided significant results, with ages not above 4.5$\,$Myr and distances compatible with the studied complex. The resulting values for the differential reddening of most candidates were relatively high, confirming that these clusters are still (partially or fully) embedded in the surrounding gas and dust, as a rule within a shell. Histograms with the distribution of the masses, ages and distances were also produced, to give an overview of the results. We conclude that all the 12 newly found embedded clusters are related to the Carina complex. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.02104v1-abstract-full').style.display = 'none'; document.getElementById('1802.02104v1-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 February, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 14 figures, accepted for publication in MNRAS</span> </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> 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