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</div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Sarajedini%2C+A&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Sarajedini%2C+A&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Sarajedini%2C+A&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Sarajedini%2C+A&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=Sarajedini%2C+A&start=150" class="pagination-link " aria-label="Page 4" aria-current="page">4 </a> </li> </ul> </nav> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.00054">arXiv:2311.00054</a> <span> [<a href="https://arxiv.org/pdf/2311.00054">pdf</a>, <a href="https://arxiv.org/format/2311.00054">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> CCD UBV and Gaia DR3 Analyses of Open Clusters King 6 and NGC 1605 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gokmen%2C+S">S. Gokmen</a>, <a href="/search/astro-ph?searchtype=author&query=Eker%2C+Z">Z. Eker</a>, <a href="/search/astro-ph?searchtype=author&query=Yontan%2C+T">T. Yontan</a>, <a href="/search/astro-ph?searchtype=author&query=Bilir%2C+S">S. Bilir</a>, <a href="/search/astro-ph?searchtype=author&query=Ak%2C+T">T. Ak</a>, <a href="/search/astro-ph?searchtype=author&query=Ak%2C+S">S. Ak</a>, <a href="/search/astro-ph?searchtype=author&query=Banks%2C+T">T. Banks</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">A. Sarajedini</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="2311.00054v1-abstract-short" style="display: inline;"> A detailed analysis of ground-based CCD UBV photometry and space-based Gaia Data Release 3 (DR3) data for the open clusters King 6 and NGC 1605 was performed. Using the pyUPMASK algorithm on Gaia astrometric data to estimate cluster membership probabilities, we have identified 112 stars in King 6 and 160 stars in NGC 1605 as the statistically most likely members of each cluster. We calculated redd… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.00054v1-abstract-full').style.display = 'inline'; document.getElementById('2311.00054v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.00054v1-abstract-full" style="display: none;"> A detailed analysis of ground-based CCD UBV photometry and space-based Gaia Data Release 3 (DR3) data for the open clusters King 6 and NGC 1605 was performed. Using the pyUPMASK algorithm on Gaia astrometric data to estimate cluster membership probabilities, we have identified 112 stars in King 6 and 160 stars in NGC 1605 as the statistically most likely members of each cluster. We calculated reddening and metallicity separately using UBV two-color diagrams to estimate parameter values via independent methods. The color excess $E(B-V)$ and photometric metallicity [Fe/H] for King 6 are $0.515 \pm 0.030$ mag and $0.02 \pm 0.20$ dex, respectively. For NGC 1605, they are $0.840 \pm 0.054$ mag and $0.01 \pm 0.20$ dex. With reddening and metallicity kept constant, we have estimated the distances and cluster ages by fitting PARSEC isochrones to color-magnitude diagrams based on the Gaia and UBV data. Photometric distances are 723 $\pm$ 34 pc for King 6 and 3054 $\pm$ 243 pc for NGC 1605. The cluster ages are $200 \pm 20$ Myr and $400 \pm 50$ Myr for King 6 and NGC 1605, respectively. Mass function slopes were found to be 1.29 $\pm$ 0.18 and 1.63 $\pm$ 0.36 for King 6 and NGC 1605, respectively. These values are in good agreement with the value of Salpeter (1955). The relaxation times were estimated as 5.8 Myr for King 6 and 60 Myr for NGC 1605. This indicates that both clusters are dynamically relaxed since these times are less than the estimated cluster ages. Galactic orbit analysis shows that both clusters formed outside the solar circle and are members of the young thin-disc population. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.00054v1-abstract-full').style.display = 'none'; document.getElementById('2311.00054v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">25 pages, including 14 figures and 7 tables, accepted for publication in the Astronomical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.12620">arXiv:2306.12620</a> <span> [<a href="https://arxiv.org/pdf/2306.12620">pdf</a>, <a href="https://arxiv.org/ps/2306.12620">ps</a>, <a href="https://arxiv.org/format/2306.12620">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Extragalactic Star Cluster Science with the Nancy Grace Roman Space Telescope's High Latitude Wide Area Survey and the Vera C. Rubin Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dage%2C+K+C">Kristen C. Dage</a>, <a href="/search/astro-ph?searchtype=author&query=Usher%2C+C">Christopher Usher</a>, <a href="/search/astro-ph?searchtype=author&query=Sobeck%2C+J">Jennifer Sobeck</a>, <a href="/search/astro-ph?searchtype=author&query=Santos%2C+A+L+C">Ana L. Chies Santos</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=Reina-Campos%2C+M">Marta Reina-Campos</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=Ripepi%2C+V">Vincenzo Ripepi</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Criscienzo%2C+M">Marcella Di Criscienzo</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">Ata Sarajedini</a>, <a href="/search/astro-ph?searchtype=author&query=Clarkson%2C+W">Will Clarkson</a>, <a href="/search/astro-ph?searchtype=author&query=McGehee%2C+P">Peregrine McGehee</a>, <a href="/search/astro-ph?searchtype=author&query=Gizis%2C+J">John Gizis</a>, <a href="/search/astro-ph?searchtype=author&query=Rhode%2C+K">Katherine Rhode</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J">John Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Theissen%2C+C+A">Christopher A. Theissen</a>, <a href="/search/astro-ph?searchtype=author&query=Calamida%2C+A">Annalisa Calamida</a>, <a href="/search/astro-ph?searchtype=author&query=Ennis%2C+A">Ana Ennis</a>, <a href="/search/astro-ph?searchtype=author&query=Chamba%2C+N">Nushkia Chamba</a>, <a href="/search/astro-ph?searchtype=author&query=Gerasimov%2C+R">Roman Gerasimov</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=Barmby%2C+P">Pauline Barmby</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=Williams%2C+B+F">Benjamin F. Williams</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="2306.12620v1-abstract-short" style="display: inline;"> The Nancy Grace Roman Telescope's High Latitude Wide Area Survey will have a number of synergies with the Vera Rubin Observatory's Legacy Survey of Space and Time (LSST), particularly for extragalactic star clusters. Understanding the nature of star clusters and star cluster systems are key topics in many areas of astronomy, chief among them stellar evolution, high energy astrophysics, galaxy asse… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.12620v1-abstract-full').style.display = 'inline'; document.getElementById('2306.12620v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.12620v1-abstract-full" style="display: none;"> The Nancy Grace Roman Telescope's High Latitude Wide Area Survey will have a number of synergies with the Vera Rubin Observatory's Legacy Survey of Space and Time (LSST), particularly for extragalactic star clusters. Understanding the nature of star clusters and star cluster systems are key topics in many areas of astronomy, chief among them stellar evolution, high energy astrophysics, galaxy assembly/dark matter, the extragalactic distance scale, and cosmology. One of the challenges will be disentangling the age/metallicity degeneracy because young ($\sim$Myr) metal-rich clusters have similar SEDs to old ($\sim$Gyr) metal-poor clusters. Rubin will provide homogeneous, $ugrizy$ photometric coverage, and measurements in the red Roman filters will help break the age-metallicity and age-extinction degeneracies, providing the first globular cluster samples that cover wide areas while essentially free of contamination from Milky Way stars. Roman's excellent spatial resolution will also allow measurements of cluster sizes. We advocate for observations of a large sample of galaxies with a range of properties and morphologies in the Rubin/LSST footprint matching the depth of the LSST Wide-Fast-Deep field $i$ band limit (26.3 mag), and recommend adding the F213 filter to the survey. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.12620v1-abstract-full').style.display = 'none'; document.getElementById('2306.12620v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 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">white paper submitted for Roman CCS input</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.04148">arXiv:2301.04148</a> <span> [<a href="https://arxiv.org/pdf/2301.04148">pdf</a>, <a href="https://arxiv.org/format/2301.04148">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/acaec6">10.3847/1538-4357/acaec6 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Hubble Space Telescope UV Legacy Survey of Galactic Globular Clusters. XXIV. Differences in internal kinematics of multiple stellar populations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Libralato%2C+M">M. Libralato</a>, <a href="/search/astro-ph?searchtype=author&query=Vesperini%2C+E">E. Vesperini</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">A. Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Milone%2C+A+P">A. P. Milone</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Marel%2C+R+P">R. P. van der Marel</a>, <a href="/search/astro-ph?searchtype=author&query=Piotto%2C+G">G. Piotto</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Aparicio%2C+A">A. Aparicio</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">B. Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=Bedin%2C+L+R">L. R. Bedin</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+T+M">T. M. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Cassisi%2C+S">S. Cassisi</a>, <a href="/search/astro-ph?searchtype=author&query=Nardiello%2C+D">D. Nardiello</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">A. Sarajedini</a>, <a href="/search/astro-ph?searchtype=author&query=Scalco%2C+M">M. Scalco</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2301.04148v2-abstract-short" style="display: inline;"> Our understanding of the kinematic properties of multiple stellar populations (mPOPs) in Galactic globular clusters (GCs) is still limited compared to what we know about their chemical and photometric characteristics. Such limitation arises from the lack of a comprehensive observational investigation of this topic. Here we present the first homogeneous kinematic analysis of mPOPs in 56 GCs based o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.04148v2-abstract-full').style.display = 'inline'; document.getElementById('2301.04148v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.04148v2-abstract-full" style="display: none;"> Our understanding of the kinematic properties of multiple stellar populations (mPOPs) in Galactic globular clusters (GCs) is still limited compared to what we know about their chemical and photometric characteristics. Such limitation arises from the lack of a comprehensive observational investigation of this topic. Here we present the first homogeneous kinematic analysis of mPOPs in 56 GCs based on high-precision proper motions computed with Hubble Space Telescope data. We focused on red-giant-branch stars, for which the mPOP tagging is clearer, and measured the velocity dispersion of stars belonging to first (1G) and second generations (2G). We find that 1G stars are generally kinematically isotropic even at the half-light radius, whereas 2G stars are isotropic at the center and become radially anisotropic before the half-light radius. The radial anisotropy is induced by a lower tangential velocity dispersion of 2G stars with respect to the 1G population, while the radial component of the motion is comparable. We also show possible evidence that the kinematic properties of mPOPs are affected by the Galactic tidal field, corroborating previous observational and theoretical results suggesting a relation between the strength of the external tidal field and some properties of mPOPs. Although limited to the GCs' central regions, our analysis leads to new insights into the mPOP phenomenon, and provides the motivation for future observational studies of the internal kinematics of mPOPs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.04148v2-abstract-full').style.display = 'none'; document.getElementById('2301.04148v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 4 figures, 2 tables. Accepted for publication on ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.05693">arXiv:2207.05693</a> <span> [<a href="https://arxiv.org/pdf/2207.05693">pdf</a>, <a href="https://arxiv.org/format/2207.05693">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/stac1758">10.1093/mnras/stac1758 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Investigating a predicted metallicity [Fe/H] variation in the Type II Globular Cluster NGC 362 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vargas%2C+C">C. Vargas</a>, <a href="/search/astro-ph?searchtype=author&query=Villanova%2C+S">S. Villanova</a>, <a href="/search/astro-ph?searchtype=author&query=Geisler%2C+D">D. Geisler</a>, <a href="/search/astro-ph?searchtype=author&query=Mu%C3%B1oz%2C+C">C. Mu帽oz</a>, <a href="/search/astro-ph?searchtype=author&query=Monaco%2C+L">L. Monaco</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Connell%2C+J">J. O'Connell</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">Ata Sarajedini</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2207.05693v1-abstract-short" style="display: inline;"> NGC 362 is a non-common Type II Galactic globular cluster, showing a complex pseudo two-color diagram or 'chromosome map'. The clear separation of its stellar populations in the color-magnitude diagram and the distribution of the giant stars in the chromosome map strongly suggests that NGC 362 could host stars with both cluster-nominal as well as enhanced heavy-element abundances, and one of them… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.05693v1-abstract-full').style.display = 'inline'; document.getElementById('2207.05693v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.05693v1-abstract-full" style="display: none;"> NGC 362 is a non-common Type II Galactic globular cluster, showing a complex pseudo two-color diagram or 'chromosome map'. The clear separation of its stellar populations in the color-magnitude diagram and the distribution of the giant stars in the chromosome map strongly suggests that NGC 362 could host stars with both cluster-nominal as well as enhanced heavy-element abundances, and one of them could be iron. However, despite previous spectroscopic observations of NGC 362, no such iron variation has been detected. Our main goal is to confirm or disprove this result by searching for any internal variation of [Fe/H] which would give us insight into the formation and evolution of this interesting globular cluster. In this paper, we present the abundance analysis for a sample of 11 red giant branch members based on high-resolution and high S/N spectra obtained with the MIKE echelle spectrograph mounted at the Magellan-Clay telescope. HST and GAIA photometry and astrometry has been used to determine atmospheric parameters and membership. We obtained T$_{\text{eff}}$, log(g) and v$_{\text{t}}$ for our target stars and measured the mean iron content of the sample and its dispersion with three different methods, which lead to [Fe/H]$_1$=-1.10$\pm0.02$, [Fe/H]$_2$=-1.09$\pm0.01$ and [Fe/H]$_3$=-1.10$\pm0.01$, while the internal dispersion turned out to be $蟽_{[\text{Fe/H}]_1}$=0.06$\pm0.01$, $蟽_{[\text{Fe/H}]_2}$=0.03$\pm0.01$ and $蟽_{[\text{Fe/H}]_3}$=0.05$\pm0.01$ respectively. The error analysis gives an internal dispersion due to observational error of 0.05 dex. Comparing the observed dispersion with the internal errors, we conclude that NGC 362 does not show any trace of an internal iron spread. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.05693v1-abstract-full').style.display = 'none'; document.getElementById('2207.05693v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 6 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/2206.09924">arXiv:2206.09924</a> <span> [<a href="https://arxiv.org/pdf/2206.09924">pdf</a>, <a href="https://arxiv.org/format/2206.09924">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac7727">10.3847/1538-4357/ac7727 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Hubble Space Telescope UV Legacy Survey of Galactic Globular Clusters. XXIII. Proper-motion catalogs and internal kinematics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Libralato%2C+M">M. Libralato</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">A. Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Vesperini%2C+E">E. Vesperini</a>, <a href="/search/astro-ph?searchtype=author&query=Piotto%2C+G">G. Piotto</a>, <a href="/search/astro-ph?searchtype=author&query=Milone%2C+A+P">A. P. Milone</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Marel%2C+R+P">R. P. van der Marel</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Aparicio%2C+A">A. Aparicio</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">B. Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=Bedin%2C+L+R">L. R. Bedin</a>, <a href="/search/astro-ph?searchtype=author&query=Borsato%2C+L">L. Borsato</a>, <a href="/search/astro-ph?searchtype=author&query=Cassisi%2C+S">S. Cassisi</a>, <a href="/search/astro-ph?searchtype=author&query=Dalessandro%2C+E">E. Dalessandro</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraro%2C+F+R">F. R. Ferraro</a>, <a href="/search/astro-ph?searchtype=author&query=King%2C+I+R">I. R. King</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzoni%2C+B">B. Lanzoni</a>, <a href="/search/astro-ph?searchtype=author&query=Nardiello%2C+D">D. Nardiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ortolani%2C+S">S. Ortolani</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">A. Sarajedini</a>, <a href="/search/astro-ph?searchtype=author&query=Sohn%2C+S+T">S. T. Sohn</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2206.09924v2-abstract-short" style="display: inline;"> A number of studies based on data collected by the $\textit{Hubble Space Telescope}$ ($\textit{HST}$) GO-13297 program "HST Legacy Survey of Galactic Globular Clusters: Shedding UV Light on Their Populations and Formation" have investigated the photometric properties of a large sample of Galactic globular clusters and revolutionized our understanding of their stellar populations. In this paper, we… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.09924v2-abstract-full').style.display = 'inline'; document.getElementById('2206.09924v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.09924v2-abstract-full" style="display: none;"> A number of studies based on data collected by the $\textit{Hubble Space Telescope}$ ($\textit{HST}$) GO-13297 program "HST Legacy Survey of Galactic Globular Clusters: Shedding UV Light on Their Populations and Formation" have investigated the photometric properties of a large sample of Galactic globular clusters and revolutionized our understanding of their stellar populations. In this paper, we expand previous studies by focusing our attention on the stellar clusters' internal kinematics. We computed proper motions for stars in 56 globular and one open clusters by combining the GO-13297 images with archival $\textit{HST}$ data. The astro-photometric catalogs released with this paper represent the most complete and homogeneous collection of proper motions of stars in the cores of stellar clusters to date, and expand the information provided by the current (and future) $\textit{Gaia}$ data releases to much fainter stars and into the crowded central regions. We also census the general kinematic properties of stellar clusters by computing the velocity-dispersion and anisotropy radial profiles of their bright members. We study the dependence on concentration and relaxation time, and derive dynamical distances. Finally, we present an in-depth kinematic analysis of the globular cluster NGC 5904. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.09924v2-abstract-full').style.display = 'none'; document.getElementById('2206.09924v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">33 pages, 19 figures, 6 tables. Accepted for publication on ApJ. Astro-photometric catalogs, velocity-dispersion values and profiles are available at https://archive.stsci.edu/hlsp/hacks</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.10853">arXiv:2109.10853</a> <span> [<a href="https://arxiv.org/pdf/2109.10853">pdf</a>, <a href="https://arxiv.org/format/2109.10853">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/stab2765">10.1093/mnras/stab2765 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Differential RR Lyrae Line-of-Sight Distance Between M31 and M33 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">Ata Sarajedini</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2109.10853v1-abstract-short" style="display: inline;"> We present a purely differential line-of-sight distance between M31 and M33 using ab-type RR Lyrae variables observed in each galaxy by the Hubble Space Telescope Advanced Camera for Surveys in the F606W filter. Using 1501 RR Lyraes in 13 M31 fields and 181 RR Lyraes in six M33 fields, and placing all of these stars on a uniform photometric scale with internally consistent corrections for metal ab… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.10853v1-abstract-full').style.display = 'inline'; document.getElementById('2109.10853v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.10853v1-abstract-full" style="display: none;"> We present a purely differential line-of-sight distance between M31 and M33 using ab-type RR Lyrae variables observed in each galaxy by the Hubble Space Telescope Advanced Camera for Surveys in the F606W filter. Using 1501 RR Lyraes in 13 M31 fields and 181 RR Lyraes in six M33 fields, and placing all of these stars on a uniform photometric scale with internally consistent corrections for metal abundance and extinction, we find a relative absolute distance modulus of D(m-M)_o = -0.298 +/- 0.016 in the sense of (m-M)_{o,M31} - (m-M)_{o,M33}. Adopting an absolute distance modulus of (m-M)_o=24.46 +/- 0.10 for M31 places M33 115 kpc beyond M31 in line-of-sight distance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.10853v1-abstract-full').style.display = 'none'; document.getElementById('2109.10853v1-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 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in the MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.15052">arXiv:2106.15052</a> <span> [<a href="https://arxiv.org/pdf/2106.15052">pdf</a>, <a href="https://arxiv.org/format/2106.15052">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/stab1891">10.1093/mnras/stab1891 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Intrinsic Metallicity Variation in the Intermediate Mass Type II Globular Cluster NGC 1261 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mu%C3%B1oz%2C+C">C茅sar Mu帽oz</a>, <a href="/search/astro-ph?searchtype=author&query=Geisler%2C+D">Douglas Geisler</a>, <a href="/search/astro-ph?searchtype=author&query=Villanova%2C+S">Sandro Villanova</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">Ata Sarajedini</a>, <a href="/search/astro-ph?searchtype=author&query=Frelijj%2C+H">Heinz Frelijj</a>, <a href="/search/astro-ph?searchtype=author&query=Vargas%2C+C">Carolina Vargas</a>, <a href="/search/astro-ph?searchtype=author&query=Monaco%2C+L">Lorenzo Monaco</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Connell%2C+J">Julia O'Connell</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2106.15052v1-abstract-short" style="display: inline;"> Globular Clusters (GCs) are now well known to almost universally show multiple popu-lations (MPs). The HST UV Legacy Survey of a large number of Galactic GCs in UV filters optimized to explore MPs finds that a small fraction of GCs, termed Type II, also display more complex, anomalous behavior. Several well-studied Type II GCs show intrinsic Fe abundance variations, suggesting that the other, less… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.15052v1-abstract-full').style.display = 'inline'; document.getElementById('2106.15052v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.15052v1-abstract-full" style="display: none;"> Globular Clusters (GCs) are now well known to almost universally show multiple popu-lations (MPs). The HST UV Legacy Survey of a large number of Galactic GCs in UV filters optimized to explore MPs finds that a small fraction of GCs, termed Type II, also display more complex, anomalous behavior. Several well-studied Type II GCs show intrinsic Fe abundance variations, suggesting that the other, less well-studied, Type II GCs should also exhibit similar behavior. Our aim is to perform the first detailed metallicity analysis of NGC 1261, an intermediate mass Type II GC, in order to determine if this object shows an intrinsic Fe variation. We determined the Fe abundance in eight red giant members using Magellan-MIKE and UVES-FLAMES high-resolution, high S/N spectroscopy. The full range of [Fe/H] for the entire sample from the spectra is from -1.05 to -1.43 dexwith an observed spread sigma_obs=0.133 dex. Compared with the total internal error of Sigma_tot=0.06,this indicates a significant intrinsic metallicity spread of Sigma_int=0.119 dex. We found a very similar variation in [Fe/H] using an independent method to derive the atmospheric parameters based on near-IR photometry. More importantly, the mean metallicity of the five presumed normal metallicity stars is -1.37+/-0.02, while that of the three presumed anomalous/highmetallicity stars is -1.18+/-0.09. This difference is significant at the $\pm$2.4Sigma level. We find indications from existing data of other Type II GCs that several of them presumedto have real metallicity spreads may in fact posses none. The minimum mass required for a GC to acquire an intrinsic Fe spread appears to be $\pm$10^5 Msun. We find no strong correlation betwee nmass and metallicity variation for Type II GCs. The metallicity spread is also independent of the fraction of anomalous stars within the Type II GCs and of GC origin. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.15052v1-abstract-full').style.display = 'none'; document.getElementById('2106.15052v1-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 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 7 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/2003.09473">arXiv:2003.09473</a> <span> [<a href="https://arxiv.org/pdf/2003.09473">pdf</a>, <a href="https://arxiv.org/format/2003.09473">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/staa822">10.1093/mnras/staa822 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Exploring the nature and synchronicity of early cluster formation in the Large Magellanic Cloud V: Multiple Populations in ancient Globular Clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gilligan%2C+C+K">Christina K. Gilligan</a>, <a href="/search/astro-ph?searchtype=author&query=Chaboyer%2C+B">Brian Chaboyer</a>, <a href="/search/astro-ph?searchtype=author&query=Cummings%2C+J+D">Jeffrey D. Cummings</a>, <a href="/search/astro-ph?searchtype=author&query=Mackey%2C+D">Dougal Mackey</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R+E">Roger E. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Geisler%2C+D">Douglas Geisler</a>, <a href="/search/astro-ph?searchtype=author&query=Grocholski%2C+A+J">Aaron J. Grocholski</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=Sarajedini%2C+A">Ata Sarajedini</a>, <a href="/search/astro-ph?searchtype=author&query=Ventura%2C+P">Paolo Ventura</a>, <a href="/search/astro-ph?searchtype=author&query=Villanova%2C+S">Sandro Villanova</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+S">Soung-Chul Yang</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="2003.09473v1-abstract-short" style="display: inline;"> We examine four ancient Large Magellanic Cloud (LMC) globular clusters (GCs) for evidence of multiple stellar populations using the Advanced Camera for Surveys and Wide Field Camera 3 on the Hubble Space Telescope Programme GO-14164. NGC 1466, NGC 1841, and NGC 2257 all show evidence for a redder, secondary population along the main-sequence. Reticulum does not show evidence for the presence of a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.09473v1-abstract-full').style.display = 'inline'; document.getElementById('2003.09473v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2003.09473v1-abstract-full" style="display: none;"> We examine four ancient Large Magellanic Cloud (LMC) globular clusters (GCs) for evidence of multiple stellar populations using the Advanced Camera for Surveys and Wide Field Camera 3 on the Hubble Space Telescope Programme GO-14164. NGC 1466, NGC 1841, and NGC 2257 all show evidence for a redder, secondary population along the main-sequence. Reticulum does not show evidence for the presence of a redder population, but this GC has the least number of stars and Monte Carlo simulations indicate that the sample of main sequence stars is too small to robustly infer whether a redder population exists in this cluster. The second, redder, population of the other three clusters constitutes $\sim30-40\%$ of the total population along the main-sequence. This brings the total number of ancient LMC GCs with known split or broadened main-sequences to five. However, unlike for Hodge 11 and NGC 2210 (see arXiv:1904.01434), none of the clusters show evidence for multiple populations in the horizontal branch. We also do not find evidence of a second population along the Red Giant Branch (RGB). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.09473v1-abstract-full').style.display = 'none'; document.getElementById('2003.09473v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 March, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2002.06479">arXiv:2002.06479</a> <span> [<a href="https://arxiv.org/pdf/2002.06479">pdf</a>, <a href="https://arxiv.org/format/2002.06479">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/stz3629">10.1093/mnras/stz3629 <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. XXI. Binaries among multiple stellar populations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Milone%2C+A+P">A. P. Milone</a>, <a href="/search/astro-ph?searchtype=author&query=Vesperini%2C+E">E. Vesperini</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=Hong%2C+J">J. Hong</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Marel%2C+R">R. van der Marel</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Renzini%2C+A">A. Renzini</a>, <a href="/search/astro-ph?searchtype=author&query=Cordoni%2C+G">G. Cordoni</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=Bellini%2C+A">A. Bellini</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=D%27Antona%2C+F">F. D'Antona</a>, <a href="/search/astro-ph?searchtype=author&query=Lagioia%2C+E+P">E. P. Lagioia</a>, <a href="/search/astro-ph?searchtype=author&query=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=Piotto%2C+G">G. Piotto</a>, <a href="/search/astro-ph?searchtype=author&query=Tailo%2C+M">M. Tailo</a>, <a href="/search/astro-ph?searchtype=author&query=Cool%2C+A">A. Cool</a>, <a href="/search/astro-ph?searchtype=author&query=Salaris%2C+M">M. Salaris</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">A. Sarajedini</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2002.06479v1-abstract-short" style="display: inline;"> A number of scenarios for the formation of multiple populations in globular clusters (GCs) predict that second generation (2G) stars form in a compact and dense subsystem embedded in a more extended first-generation (1G) system. If these scenarios are accurate, a consequence of the denser 2G formation environment is that 2G binaries should be more significantly affected by stellar interactions and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.06479v1-abstract-full').style.display = 'inline'; document.getElementById('2002.06479v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2002.06479v1-abstract-full" style="display: none;"> A number of scenarios for the formation of multiple populations in globular clusters (GCs) predict that second generation (2G) stars form in a compact and dense subsystem embedded in a more extended first-generation (1G) system. If these scenarios are accurate, a consequence of the denser 2G formation environment is that 2G binaries should be more significantly affected by stellar interactions and disrupted at a larger rate than 1G binaries. The fractions and properties of binary stars can thus provide a dynamical fingerprint of the formation epoch of multiple-population GCs and their subsequent dynamical evolution. We investigate the connection between binaries and multiple populations in five GCs, NGC 288, NGC 6121 (M 4), NGC 6352, NGC 6362, and NGC 6838 (M 71). To do this, we introduce a new method based on the comparison of Hubble Space Telescope observations of binaries in the F275W, F336W, F438W, F606W and F814W filters with a large number of simulated binaries. In the inner regions probed by our data we do not find large differences between the local 1G and the 2G binary incidences in four of the studied clusters, the only exception being M 4 where the 1G binary incidence is about three times larger than the 2G incidence. The results found are in general agreement with the results of simulations predicting significant differences in the global 1G and 2G incidences and in the local values in the clusters' outer regions but similar incidences in the inner regions. The significant difference found in M 4 is consistent with simulations with a larger fraction of wider binaries. Our analysis also provides the first evidence of mixed (1G-2G) binaries, a population predicted by numerical simulations to form in a cluster's inner regions as a result of stellar encounters during which one component of a binary is replaced by a star of a different population. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.06479v1-abstract-full').style.display = 'none'; document.getElementById('2002.06479v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 February, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 11 figures, published in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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/1910.01773">arXiv:1910.01773</a> <span> [<a href="https://arxiv.org/pdf/1910.01773">pdf</a>, <a href="https://arxiv.org/format/1910.01773">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/stz2814">10.1093/mnras/stz2814 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Standard Galactic Field RR Lyrae II: A Gaia DR2 calibration of the period-Wesenheit-metallicity relation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Neeley%2C+J+R">Jillian R. Neeley</a>, <a href="/search/astro-ph?searchtype=author&query=Marengo%2C+M">Massimo Marengo</a>, <a href="/search/astro-ph?searchtype=author&query=Freedman%2C+W+L">Wendy L. Freedman</a>, <a href="/search/astro-ph?searchtype=author&query=Madore%2C+B+F">Barry F. Madore</a>, <a href="/search/astro-ph?searchtype=author&query=Beaton%2C+R+L">Rachael L. Beaton</a>, <a href="/search/astro-ph?searchtype=author&query=Hatt%2C+D">Dylan Hatt</a>, <a href="/search/astro-ph?searchtype=author&query=Hoyt%2C+T">Taylor Hoyt</a>, <a href="/search/astro-ph?searchtype=author&query=Monson%2C+A+J">Andrew J. Monson</a>, <a href="/search/astro-ph?searchtype=author&query=Rich%2C+J+A">Jeffrey A. Rich</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">Ata Sarajedini</a>, <a href="/search/astro-ph?searchtype=author&query=Seibert%2C+M">Mark Seibert</a>, <a href="/search/astro-ph?searchtype=author&query=Scowcroft%2C+V">Victoria Scowcroft</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1910.01773v2-abstract-short" style="display: inline;"> RR Lyrae stars have long been popular standard candles, but significant advances in methodology and technology have been made in recent years to increase their precision as distance indicators. We present multi-wavelength (optical $UBVR_cI_c$ and Gaia $G, BP, RP$; near-infrared $JHK_s$; mid-infrared $[3.6], [4.5]$) period-luminosity-metallicity (PLZ), period-Wesenheit-metallicity (PWZ) relations,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.01773v2-abstract-full').style.display = 'inline'; document.getElementById('1910.01773v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1910.01773v2-abstract-full" style="display: none;"> RR Lyrae stars have long been popular standard candles, but significant advances in methodology and technology have been made in recent years to increase their precision as distance indicators. We present multi-wavelength (optical $UBVR_cI_c$ and Gaia $G, BP, RP$; near-infrared $JHK_s$; mid-infrared $[3.6], [4.5]$) period-luminosity-metallicity (PLZ), period-Wesenheit-metallicity (PWZ) relations, calibrated using photometry obtained from The Carnegie RR Lyrae Program and parallaxes from the Gaia second data release for 55 Galactic field RR Lyrae stars. The metallicity slope, which has long been predicted by theoretical relations, can now be measured in all passbands. The scatter in the PLZ relations is on the order of 0.2 mag, and is still dominated by uncertainties in the parallaxes. As a consistency check of our PLZ relations, we also measure the distance modulus to the globular cluster M4, the Large Magellanic Cloud (LMC) and the Small Magellanic Cloud (SMC), and our results are in excellent agreement with estimates from previous studies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.01773v2-abstract-full').style.display = 'none'; document.getElementById('1910.01773v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 October, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 October, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in MNRAS, 15 pages, 14 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/1904.01434">arXiv:1904.01434</a> <span> [<a href="https://arxiv.org/pdf/1904.01434">pdf</a>, <a href="https://arxiv.org/format/1904.01434">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/stz1174">10.1093/mnras/stz1174 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Exploring the nature and synchronicity of early cluster formation in the Large Magellanic Cloud IV: Evidence for Multiple Populations in Hodge 11 and NGC 2210 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gilligan%2C+C+K">Christina K. Gilligan</a>, <a href="/search/astro-ph?searchtype=author&query=Chaboyer%2C+B">Brian Chaboyer</a>, <a href="/search/astro-ph?searchtype=author&query=Cummings%2C+J+D">Jeffrey D. Cummings</a>, <a href="/search/astro-ph?searchtype=author&query=Mackey%2C+D">Dougal Mackey</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R+E">Roger E. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Geisler%2C+D">Doug Geisler</a>, <a href="/search/astro-ph?searchtype=author&query=Grocholski%2C+A+J">Aaron J. Grocholski</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=Sarajedini%2C+A">Ata Sarajedini</a>, <a href="/search/astro-ph?searchtype=author&query=Ventura%2C+P">Paolo Ventura</a>, <a href="/search/astro-ph?searchtype=author&query=Villanova%2C+S">Sandro Villanova</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+S">Soung-Chul Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Wagner-Kaiser%2C+R">Rachel Wagner-Kaiser</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1904.01434v2-abstract-short" style="display: inline;"> We present a multiple population search in two old Large Magellanic Cloud (LMC) Globular Clusters, Hodge 11 and NGC 2210. This work uses data from the Advanced Camera for Surveys and Wide Field Camera 3 on the Hubble Space Telescope from programme GO-14164 in Cycle 23. Both of these clusters exhibit a broadened main sequence with the second population representing ($20 \pm \! \sim \! 5$)% for NGC… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.01434v2-abstract-full').style.display = 'inline'; document.getElementById('1904.01434v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1904.01434v2-abstract-full" style="display: none;"> We present a multiple population search in two old Large Magellanic Cloud (LMC) Globular Clusters, Hodge 11 and NGC 2210. This work uses data from the Advanced Camera for Surveys and Wide Field Camera 3 on the Hubble Space Telescope from programme GO-14164 in Cycle 23. Both of these clusters exhibit a broadened main sequence with the second population representing ($20 \pm \! \sim \! 5$)% for NGC 2210 and ($30 \pm \! \sim \! 5$)% for Hodge 11. In both clusters, the smaller population is redder than the primary population, suggesting CNO variations. Hodge 11 also displays a bluer second population in the horizontal branch, which is evidence for helium enhancement. However, even though NGC 2210 shows similarities to Hodge 11 in the main sequence, there does not appear to be a second population on NGC 2210's horizontal branch. This is the first photometric evidence that ancient LMC Globular Clusters exhibit multiple stellar populations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.01434v2-abstract-full').style.display = 'none'; document.getElementById('1904.01434v2-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 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 19 figures, submitted to MNRAS, deleted one sentence and fixed Figure 2 which had the same plot twice</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1809.05006">arXiv:1809.05006</a> <span> [<a href="https://arxiv.org/pdf/1809.05006">pdf</a>, <a href="https://arxiv.org/ps/1809.05006">ps</a>, <a href="https://arxiv.org/format/1809.05006">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/sty2573">10.1093/mnras/sty2573 <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. XVI. The helium abundance of multiple populations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Milone%2C+A+P">A. P. Milone</a>, <a href="/search/astro-ph?searchtype=author&query=Marino%2C+A+F">A. F. Marino</a>, <a href="/search/astro-ph?searchtype=author&query=Renzini%2C+A">A. Renzini</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=Anderson%2C+J">J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">B. Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=Bedin%2C+L+R">L. R. Bedin</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">A. Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+T+M">T. M. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Cassisi%2C+S">S. Cassisi</a>, <a href="/search/astro-ph?searchtype=author&query=Cordoni%2C+G">G. Cordoni</a>, <a href="/search/astro-ph?searchtype=author&query=Lagioia%2C+E+P">E. P. Lagioia</a>, <a href="/search/astro-ph?searchtype=author&query=Nardiello%2C+D">D. Nardiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ortolani%2C+S">S. Ortolani</a>, <a href="/search/astro-ph?searchtype=author&query=Piotto%2C+G">G. Piotto</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">A. Sarajedini</a>, <a href="/search/astro-ph?searchtype=author&query=Tailo%2C+M">M. Tailo</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Marel%2C+R+P">R. P. van der Marel</a>, <a href="/search/astro-ph?searchtype=author&query=Vesperini%2C+E">E. Vesperini</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1809.05006v1-abstract-short" style="display: inline;"> Recent work, based on data from the Hubble Space Telescope (HST) UV Legacy Survey of Galactic Globular Clusters (GCs), has revealed that all the analyzed clusters host two groups of first- (1G) and second-generation (2G) stars. In most GCs, both 1G and 2G stars host sub-stellar populations with different chemical composition. We compare multi-wavelength HST photometry with synthetic spectra to det… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1809.05006v1-abstract-full').style.display = 'inline'; document.getElementById('1809.05006v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1809.05006v1-abstract-full" style="display: none;"> Recent work, based on data from the Hubble Space Telescope (HST) UV Legacy Survey of Galactic Globular Clusters (GCs), has revealed that all the analyzed clusters host two groups of first- (1G) and second-generation (2G) stars. In most GCs, both 1G and 2G stars host sub-stellar populations with different chemical composition. We compare multi-wavelength HST photometry with synthetic spectra to determine for the first time the average helium difference between the 2G and 1G stars in a large sample of 57 GCs and the maximum helium variation within each of them. We find that in all clusters 2G stars are consistent with being enhanced in helium with respect to 1G. The maximum helium variation ranges from less than 0.01 to more than 0.10 in helium mass fraction and correlates with both the cluster mass and the color extension of the horizontal branch (HB). These findings demonstrate that the internal helium variation is one of the main (second) parameters governing the HB morphology. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1809.05006v1-abstract-full').style.display = 'none'; document.getElementById('1809.05006v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 September, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">26 pages, 19 figures, accepted for publications 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/1808.05582">arXiv:1808.05582</a> <span> [<a href="https://arxiv.org/pdf/1808.05582">pdf</a>, <a href="https://arxiv.org/format/1808.05582">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/aae08f">10.3847/2041-8213/aae08f <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Ruprecht 106: A riddle, wrapped in a mystery, inside an enigma </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dotter%2C+A">Aaron Dotter</a>, <a href="/search/astro-ph?searchtype=author&query=Milone%2C+A+P">Antonino P. Milone</a>, <a href="/search/astro-ph?searchtype=author&query=Conroy%2C+C">Charlie Conroy</a>, <a href="/search/astro-ph?searchtype=author&query=Marino%2C+A+F">Anna F. Marino</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">Ata Sarajedini</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="1808.05582v2-abstract-short" style="display: inline;"> Galactic globular clusters (GCs) show overwhelming photometric and spectroscopic evidence for the existence of multiple stellar populations. The question of whether or not there exists a GC that represents a true 'simple stellar population' remains open. Here we focus on Ruprecht 106 (R106), a halo GC with [Fe/H]=-1.5 and [alpha/Fe]~0. A previous spectroscopic study found no sign of the Na-O antic… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.05582v2-abstract-full').style.display = 'inline'; document.getElementById('1808.05582v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1808.05582v2-abstract-full" style="display: none;"> Galactic globular clusters (GCs) show overwhelming photometric and spectroscopic evidence for the existence of multiple stellar populations. The question of whether or not there exists a GC that represents a true 'simple stellar population' remains open. Here we focus on Ruprecht 106 (R106), a halo GC with [Fe/H]=-1.5 and [alpha/Fe]~0. A previous spectroscopic study found no sign of the Na-O anticorrelation among 9 of its brightest red giants, which led to the conclusion that R106 is a true simple stellar population GC. Here we present new Hubble Space Telescope (HST) Wide Field Camera 3 photometry of R106 that, when combined with archival HST images spanning a 6-year baseline, allows us to create proper motion cleaned color-magnitude diagrams spanning the ultraviolet (F336W) to the near-infrared (F814W). These data allow us to construct the pseudo-color C_{U,B,I} that is sensitive to the presence of light-element abundance spreads. We find no evidence of a split along the red giant branch (RGB) in the C_{U,B,I} diagram but the width of the RGB (sigma_CUBI = 0.015) is marginally broader than expected from artificial star tests (sigma_CUBI = 0.009). The observed spread in C_{U,B,I} is smaller than any other Galactic GC studied to date. Our results raise important questions about the role of formation environment and primordial chemical composition in the formation of multiple stellar populations in GCs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.05582v2-abstract-full').style.display = 'none'; document.getElementById('1808.05582v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 September, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 August, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">11 pages, 5 figures, accepted version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2018, ApJL, 865, 1 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1808.05271">arXiv:1808.05271</a> <span> [<a href="https://arxiv.org/pdf/1808.05271">pdf</a>, <a href="https://arxiv.org/format/1808.05271">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/aadb43">10.3847/1538-4357/aadb43 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The GeMS/GSAOI Galactic Globular Cluster Survey (G4CS) I: A Pilot Study of the stellar populations in NGC 2298 and NGC 3201 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Monty%2C+S">Stephanie Monty</a>, <a href="/search/astro-ph?searchtype=author&query=Puzia%2C+T+H">Thomas H. Puzia</a>, <a href="/search/astro-ph?searchtype=author&query=Miller%2C+B+W">Bryan W. Miller</a>, <a href="/search/astro-ph?searchtype=author&query=Carrasco%2C+E+R">Eleazar R. Carrasco</a>, <a href="/search/astro-ph?searchtype=author&query=Simunovic%2C+M">Mirko Simunovic</a>, <a href="/search/astro-ph?searchtype=author&query=Schirmer%2C+M">Mischa Schirmer</a>, <a href="/search/astro-ph?searchtype=author&query=Stetson%2C+P+B">Peter B. Stetson</a>, <a href="/search/astro-ph?searchtype=author&query=Cassisi%2C+S">Santi Cassisi</a>, <a href="/search/astro-ph?searchtype=author&query=Venn%2C+K+A">Kim A. Venn</a>, <a href="/search/astro-ph?searchtype=author&query=Dotter%2C+A">Aaron Dotter</a>, <a href="/search/astro-ph?searchtype=author&query=Goudfrooij%2C+P">Paul Goudfrooij</a>, <a href="/search/astro-ph?searchtype=author&query=Perina%2C+S">Sibilla Perina</a>, <a href="/search/astro-ph?searchtype=author&query=Pessev%2C+P">Peter Pessev</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">Ata Sarajedini</a>, <a href="/search/astro-ph?searchtype=author&query=Taylor%2C+M+A">Matthew A. Taylor</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="1808.05271v1-abstract-short" style="display: inline;"> We present the first results from the GeMS/GSAOI Galactic Globular Cluster Survey (G4CS) of the Milky-Way globular clusters (GCs) NGC 3201 and NGC 2298. Using the Gemini South Adaptive Optics Imager (GSAOI), in tandem with the Gemini Multi-conjugate adaptive optics System (GeMS) on the 8.1-meter Gemini-South telescope, we collected deep near-IR observations of both clusters, resolving their consti… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.05271v1-abstract-full').style.display = 'inline'; document.getElementById('1808.05271v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1808.05271v1-abstract-full" style="display: none;"> We present the first results from the GeMS/GSAOI Galactic Globular Cluster Survey (G4CS) of the Milky-Way globular clusters (GCs) NGC 3201 and NGC 2298. Using the Gemini South Adaptive Optics Imager (GSAOI), in tandem with the Gemini Multi-conjugate adaptive optics System (GeMS) on the 8.1-meter Gemini-South telescope, we collected deep near-IR observations of both clusters, resolving their constituent stellar populations down to $K_s\simeq21$ Vega mag. Point spread function (PSF) photometry was performed on the data using spatially-variable PSFs to generate $JHK_{s}$ photometric catalogues for both clusters. These catalogues were combined with Hubble Space Telescope (HST) data to augment the photometric wavelength coverage, yielding catalogues that span the near-ultraviolet (UV) to near-infrared (near-IR). We then applied 0.14 mas/year accurate proper-motion cleaning, differential-reddening corrections and chose to anchor our isochrones using the lower main-sequence knee (MSK) and the main-sequence turn-off (MSTO) prior to age determination. As a result of the data quality, we found that the $K_{s}$ vs. F606W$-K_{s}$ and F336W vs. F336W$-K_{s}$ color-magnitude diagrams (CMDs) were the most diagnostically powerful. We used these two color combinations to derive the stellar-population ages, distances and reddening values for both clusters. Following isochrone-fitting using three different isochrone sets, we derived best-fit absolute ages of $12.2\pm0.5$ Gyr and $13.2\pm0.4$ Gyr for NGC 3201 and NGC 2298, respectively. This was done using a weighted average over the two aforementioned color combinations, following a pseudo-$蠂^2$ determination of the best-fit isochrone set. Our derived parameters are in good agreement with recent age determinations of the two clusters, with our constraints on the ages being or ranking among the most statistically robust. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.05271v1-abstract-full').style.display = 'none'; document.getElementById('1808.05271v1-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 August, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in The Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1805.11150">arXiv:1805.11150</a> <span> [<a href="https://arxiv.org/pdf/1805.11150">pdf</a>, <a href="https://arxiv.org/ps/1805.11150">ps</a>, <a href="https://arxiv.org/format/1805.11150">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/aac889">10.3847/1538-3881/aac889 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Deep Hubble Space Telescope Imaging of Globular Clusters Towards the Galactic Bulge: Observations, Data Reduction and Color-Magnitude Diagrams </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R+E">Roger E. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Mauro%2C+F">Francesco Mauro</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso-Garc%C3%ADa%2C+J">Javier Alonso-Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Hempel%2C+M">Maren Hempel</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">Ata Sarajedini</a>, <a href="/search/astro-ph?searchtype=author&query=Ordo%C3%B1ez%2C+A+J">Antonio J. Ordo帽ez</a>, <a href="/search/astro-ph?searchtype=author&query=Geisler%2C+D">Douglas Geisler</a>, <a href="/search/astro-ph?searchtype=author&query=Kalirai%2C+J+S">Jason S. Kalirai</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1805.11150v1-abstract-short" style="display: inline;"> The Galactic globular clusters (GGCs) located towards the Galactic bulge have generally been excluded from large-scale photometric GGC surveys due to severe total and differential extinction. Here, we present an overview of a Hubble Space Telescope program designed to obtain deep, high spatial resolution multiband imaging of 16 poorly studied GGCs located towards the inner Galactic bulge and disk.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.11150v1-abstract-full').style.display = 'inline'; document.getElementById('1805.11150v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1805.11150v1-abstract-full" style="display: none;"> The Galactic globular clusters (GGCs) located towards the Galactic bulge have generally been excluded from large-scale photometric GGC surveys due to severe total and differential extinction. Here, we present an overview of a Hubble Space Telescope program designed to obtain deep, high spatial resolution multiband imaging of 16 poorly studied GGCs located towards the inner Galactic bulge and disk. In this first paper of a series resulting from these observations, we give an overview of target cluster selection, observations and data reduction procedures for optimizing the resulting photometric catalogs. Artificial star tests are used to compare the respective advantages of different data reduction strategies in terms of photometric and astrometric precision and photometric incompleteness. We present the resulting color-magnitude diagrams (CMDs) of all target clusters in several color-magnitude planes, along with CMDs of comparison fields from parallel observations. For each target cluster, we summarize existing studies, and discuss their CMDs qualitatively in the context of these results. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.11150v1-abstract-full').style.display = 'none'; document.getElementById('1805.11150v1-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 May, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">AJ accepted. Figure quality has been reduced to meet arXiv size limits</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1801.03395">arXiv:1801.03395</a> <span> [<a href="https://arxiv.org/pdf/1801.03395">pdf</a>, <a href="https://arxiv.org/ps/1801.03395">ps</a>, <a href="https://arxiv.org/format/1801.03395">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/sty083">10.1093/mnras/sty083 <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 - XII. The RGB Bumps of multiple stellar populations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lagioia%2C+E+P">E. P. Lagioia</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=Marino%2C+A+F">A. F. Marino</a>, <a href="/search/astro-ph?searchtype=author&query=Cassisi%2C+S">S. Cassisi</a>, <a href="/search/astro-ph?searchtype=author&query=Aparicio%2C+A+J">A. J. Aparicio</a>, <a href="/search/astro-ph?searchtype=author&query=Piotto%2C+G">G. Piotto</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">B. Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=Bedin%2C+L+R">L. R. Bedin</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">A. Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+T">T. Brown</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=Nardiello%2C+D">D. Nardiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ortolani%2C+S">S. Ortolani</a>, <a href="/search/astro-ph?searchtype=author&query=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=Salaris%2C+M">M. Salaris</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>, <a href="/search/astro-ph?searchtype=author&query=Vesperini%2C+E">E. Vesperini</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1801.03395v1-abstract-short" style="display: inline;"> The Hubble Space Telescope UV Legacy Survey of Galactic Globular Clusters is providing a major breakthrough in our knowledge of Globular Clusters (GCs) and their stellar populations. Among the main results, we discovered that all the studied GCs host two main discrete groups consisting of first generation (1G) and second generation (2G) stars. We exploit the multiwavelength photometry from this pr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.03395v1-abstract-full').style.display = 'inline'; document.getElementById('1801.03395v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1801.03395v1-abstract-full" style="display: none;"> The Hubble Space Telescope UV Legacy Survey of Galactic Globular Clusters is providing a major breakthrough in our knowledge of Globular Clusters (GCs) and their stellar populations. Among the main results, we discovered that all the studied GCs host two main discrete groups consisting of first generation (1G) and second generation (2G) stars. We exploit the multiwavelength photometry from this project to investigate, for the first time, the Red Giant Branch Bump (RGBB) of the two generations in a large sample of GCs. We identified, with high statistical significance, the RGBB of 1G and 2G stars in 26 GCs and found that their magnitude separation as a function of the filter wavelength follows comparable trends. The comparison of observations to synthetic spectra reveals that the RGBB luminosity depends on the stellar chemical composition and that the 2G RGBB is consistent with stars enhanced in He and N and depleted in C and O with respect to 1G stars. For metal-poor GCs the 1G and 2G RGBB relative luminosity in optical bands mostly depends on helium content, Y. We used the RGBB observations in F606W and F814W bands to infer the relative helium abundance of 1G and 2G stars in 18 GCs, finding an average helium enhancement $螖$Y=0.011$\pm$0.002 of 2G stars with respect to 1G stars. This is the first determination of the average difference in helium abundance of multiple populations in a large number of clusters and provides a lower limit to the maximum internal variation of helium in GCs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.03395v1-abstract-full').style.display = 'none'; document.getElementById('1801.03395v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 January, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">16 pages, 11 figures, 2 tables. Accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1801.00006">arXiv:1801.00006</a> <span> [<a href="https://arxiv.org/pdf/1801.00006">pdf</a>, <a href="https://arxiv.org/format/1801.00006">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/stx3061">10.1093/mnras/stx3061 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Exploring the nature and synchronicity of early cluster formation in the Large Magellanic Cloud: III. Horizontal Branch Morphology </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wagner-Kaiser%2C+R">R. Wagner-Kaiser</a>, <a href="/search/astro-ph?searchtype=author&query=Mackey%2C+D">Dougal Mackey</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">Ata Sarajedini</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R+E">Roger E. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Geisler%2C+D">Doug Geisler</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+S">Soung-Chul Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Grocholski%2C+A+J">Aaron J. Grocholski</a>, <a href="/search/astro-ph?searchtype=author&query=Cummings%2C+J+D">Jeffrey D. Cummings</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="1801.00006v1-abstract-short" style="display: inline;"> We leverage new high-quality data from Hubble Space Telescope program GO-14164 to explore the variation in horizontal branch morphology among globular clusters in the Large Magellanic Cloud (LMC). Our new observations lead to photometry with a precision commensurate with that available for the Galactic globular cluster population. Our analysis indicates that, once metallicity is accounted for, clu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.00006v1-abstract-full').style.display = 'inline'; document.getElementById('1801.00006v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1801.00006v1-abstract-full" style="display: none;"> We leverage new high-quality data from Hubble Space Telescope program GO-14164 to explore the variation in horizontal branch morphology among globular clusters in the Large Magellanic Cloud (LMC). Our new observations lead to photometry with a precision commensurate with that available for the Galactic globular cluster population. Our analysis indicates that, once metallicity is accounted for, clusters in the LMC largely share similar horizontal branch morphologies regardless of their location within the system. Furthermore, the LMC clusters possess, on average, slightly redder morphologies than most of the inner halo Galactic population; we find, instead, that their characteristics tend to be more similar to those exhibited by clusters in the outer Galactic halo. Our results are consistent with previous studies showing a correlation between horizontal branch morphology and age. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.00006v1-abstract-full').style.display = 'none'; document.getElementById('1801.00006v1-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 December, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted 2017 November 22. Received 2017 October 31; in original form 2017 August 5. 9 pages, 7 figures, 3 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1709.05542">arXiv:1709.05542</a> <span> [<a href="https://arxiv.org/pdf/1709.05542">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> CIRCE: The Canarias InfraRed Camera Experiment for the Gran Telescopio Canarias </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Eikenberry%2C+S+S">Stephen S. Eikenberry</a>, <a href="/search/astro-ph?searchtype=author&query=Charcos%2C+M">Miguel Charcos</a>, <a href="/search/astro-ph?searchtype=author&query=Edwards%2C+M+L">Michelle L. Edwards</a>, <a href="/search/astro-ph?searchtype=author&query=Garner%2C+A">Alan Garner</a>, <a href="/search/astro-ph?searchtype=author&query=Lasso-Cabrera%2C+N">Nestor Lasso-Cabrera</a>, <a href="/search/astro-ph?searchtype=author&query=Stelter%2C+R+D">Richard D. Stelter</a>, <a href="/search/astro-ph?searchtype=author&query=Marin-Franch%2C+A">Antonio Marin-Franch</a>, <a href="/search/astro-ph?searchtype=author&query=Raines%2C+S+N">S. Nicholas Raines</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">Kendall Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+J+G">John G. Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Cenarro%2C+J+A">Javier A. Cenarro</a>, <a href="/search/astro-ph?searchtype=author&query=Chinn%2C+B">Brian Chinn</a>, <a href="/search/astro-ph?searchtype=author&query=Donoso%2C+H+V">H. Veronica Donoso</a>, <a href="/search/astro-ph?searchtype=author&query=Frommeyer%2C+R">Raymond Frommeyer</a>, <a href="/search/astro-ph?searchtype=author&query=Hanna%2C+K">Kevin Hanna</a>, <a href="/search/astro-ph?searchtype=author&query=Herlevich%2C+M+D">Michael D. Herlevich</a>, <a href="/search/astro-ph?searchtype=author&query=Julian%2C+J">Jeff Julian</a>, <a href="/search/astro-ph?searchtype=author&query=Miller%2C+P">Paola Miller</a>, <a href="/search/astro-ph?searchtype=author&query=Mullin%2C+S">Scott Mullin</a>, <a href="/search/astro-ph?searchtype=author&query=Murphey%2C+C+H">Charles H. Murphey</a>, <a href="/search/astro-ph?searchtype=author&query=Packham%2C+C">Chris Packham</a>, <a href="/search/astro-ph?searchtype=author&query=Varosi%2C+F">Frank Varosi</a>, <a href="/search/astro-ph?searchtype=author&query=Vega%2C+C">Claudia Vega</a>, <a href="/search/astro-ph?searchtype=author&query=Warner%2C+C">Craig Warner</a>, <a href="/search/astro-ph?searchtype=author&query=Ramaprakash%2C+A+N">A. N. Ramaprakash</a> , et al. (29 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="1709.05542v1-abstract-short" style="display: inline;"> The Canarias InfraRed Camera Experiment (CIRCE) is a near-infrared (1-2.5 micron) imager, polarimeter and low-resolution spectrograph operating as a visitor instrument for the Gran Telescopio Canarias 10.4-meter telescope. It was designed and built largely by graduate students and postdocs, with help from the UF astronomy engineering group, and is funded by the University of Florida and the U.S. N… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1709.05542v1-abstract-full').style.display = 'inline'; document.getElementById('1709.05542v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1709.05542v1-abstract-full" style="display: none;"> The Canarias InfraRed Camera Experiment (CIRCE) is a near-infrared (1-2.5 micron) imager, polarimeter and low-resolution spectrograph operating as a visitor instrument for the Gran Telescopio Canarias 10.4-meter telescope. It was designed and built largely by graduate students and postdocs, with help from the UF astronomy engineering group, and is funded by the University of Florida and the U.S. National Science Foundation. CIRCE is intended to help fill the gap in near-infrared capabilities prior to the arrival of EMIR to the GTC, and will also provide the following scientific capabilities to compliment EMIR after its arrival: high-resolution imaging, narrowband imaging, high-time-resolution photometry, imaging polarimetry, low resolution spectroscopy. In this paper, we review the design, fabrication, integration, lab testing, and on-sky performance results for CIRCE. These include a novel approach to the opto-mechanical design, fabrication, and alignment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1709.05542v1-abstract-full').style.display = 'none'; document.getElementById('1709.05542v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 September, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">41 pages, 18 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1707.01571">arXiv:1707.01571</a> <span> [<a href="https://arxiv.org/pdf/1707.01571">pdf</a>, <a href="https://arxiv.org/format/1707.01571">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/stx1702">10.1093/mnras/stx1702 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Exploring the nature and synchronicity of early cluster formation in the Large Magellanic Cloud: II. Relative ages and distances for six ancient globular clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wagner-Kaiser%2C+R">R. Wagner-Kaiser</a>, <a href="/search/astro-ph?searchtype=author&query=Mackey%2C+D">Dougal Mackey</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">Ata Sarajedini</a>, <a href="/search/astro-ph?searchtype=author&query=Chaboyer%2C+B">Brian Chaboyer</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R+E">Roger E. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+S">Soung-Chul Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Cummings%2C+J+D">Jeffrey D. Cummings</a>, <a href="/search/astro-ph?searchtype=author&query=Geisler%2C+D">Doug Geisler</a>, <a href="/search/astro-ph?searchtype=author&query=Grocholski%2C+A+J">Aaron J. Grocholski</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="1707.01571v1-abstract-short" style="display: inline;"> We analyze Hubble Space Telescope observations of six globular clusters in the Large Magellanic Cloud from program GO-14164 in Cycle 23. These are the deepest available observations of the LMC globular cluster population; their uniformity facilitates a precise comparison with globular clusters in the Milky Way. Measuring the magnitude of the main sequence turnoff point relative to template Galacti… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.01571v1-abstract-full').style.display = 'inline'; document.getElementById('1707.01571v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1707.01571v1-abstract-full" style="display: none;"> We analyze Hubble Space Telescope observations of six globular clusters in the Large Magellanic Cloud from program GO-14164 in Cycle 23. These are the deepest available observations of the LMC globular cluster population; their uniformity facilitates a precise comparison with globular clusters in the Milky Way. Measuring the magnitude of the main sequence turnoff point relative to template Galactic globular clusters allows the relative ages of the clusters to be determined with a mean precision of 8.4%, and down to 6% for individual objects. We find that the mean age of our LMC cluster ensemble is identical to the mean age of the oldest metal-poor clusters in the Milky Way halo to 0.2 $\pm$ 0.4 Gyr. This provides the most sensitive test to date of the synchronicity of the earliest epoch of globular cluster formation in two independent galaxies. Horizontal branch magnitudes and subdwarf fitting to the main sequence allow us to determine distance estimates for each cluster, and examine their geometric distribution in the LMC. Using two different methods, we find an average distance to the LMC of 18.52 $\pm$ 0.05. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.01571v1-abstract-full').style.display = 'none'; document.getElementById('1707.01571v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 July, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted at MNRAS, 13 pages, 9 figures, 6 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1702.08856">arXiv:1702.08856</a> <span> [<a href="https://arxiv.org/pdf/1702.08856">pdf</a>, <a href="https://arxiv.org/format/1702.08856">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/stx544">10.1093/mnras/stx544 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The ACS Survey of Galactic Globular Clusters XIV: Bayesian Single-Population Analysis of 69 Globular Clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wagner-Kaiser%2C+R">R. Wagner-Kaiser</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">A. Sarajedini</a>, <a href="/search/astro-ph?searchtype=author&query=von+Hippel%2C+T">T. von Hippel</a>, <a href="/search/astro-ph?searchtype=author&query=Stenning%2C+D+C">D. C. Stenning</a>, <a href="/search/astro-ph?searchtype=author&query=van+Dyk%2C+D+A">D. A. van Dyk</a>, <a href="/search/astro-ph?searchtype=author&query=Jeffery%2C+E">E. Jeffery</a>, <a href="/search/astro-ph?searchtype=author&query=Robinson%2C+E">E. Robinson</a>, <a href="/search/astro-ph?searchtype=author&query=Stein%2C+N">N. Stein</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Jefferys%2C+W+H">W. H. Jefferys</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="1702.08856v1-abstract-short" style="display: inline;"> We use Hubble Space Telescope (HST) imaging from the ACS Treasury Survey to determine fits for single population isochrones of 69 Galactic globular clusters. Using robust Bayesian analysis techniques, we simultaneously determine ages, distances, absorptions, and helium values for each cluster under the scenario of a "single" stellar population on model grids with solar ratio heavy element abundanc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1702.08856v1-abstract-full').style.display = 'inline'; document.getElementById('1702.08856v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1702.08856v1-abstract-full" style="display: none;"> We use Hubble Space Telescope (HST) imaging from the ACS Treasury Survey to determine fits for single population isochrones of 69 Galactic globular clusters. Using robust Bayesian analysis techniques, we simultaneously determine ages, distances, absorptions, and helium values for each cluster under the scenario of a "single" stellar population on model grids with solar ratio heavy element abundances. The set of cluster parameters is determined in a consistent and reproducible manner for all clusters using the Bayesian analysis suite BASE-9. Our results are used to re-visit the age-metallicity relation. We find correlations with helium and several other parameters such as metallicity, binary fraction, and proxies for cluster mass. The helium abundances of the clusters are also considered in the context of CNO abundances and the multiple population scenario. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1702.08856v1-abstract-full').style.display = 'none'; document.getElementById('1702.08856v1-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 February, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted: MNRAS 20 pages, 13 figures, 5 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1702.00803">arXiv:1702.00803</a> <span> [<a href="https://arxiv.org/pdf/1702.00803">pdf</a>, <a href="https://arxiv.org/format/1702.00803">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/10.3847/1538-4357/835/2/152">10.3847/1538-4357/835/2/152 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Testing Metal Poor Stellar Models and Isochrones with HST Parallaxes of Metal Poor Stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chaboyer%2C+B">B. Chaboyer</a>, <a href="/search/astro-ph?searchtype=author&query=McArthur%2C+B+E">B. E. McArthur</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Malley%2C+E">E. O'Malley</a>, <a href="/search/astro-ph?searchtype=author&query=Benedict%2C+G+F">G. F. Benedict</a>, <a href="/search/astro-ph?searchtype=author&query=Feiden%2C+G+A">G. A. Feiden</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+T+E">T. E. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=McWilliam%2C+A">A. McWilliam</a>, <a href="/search/astro-ph?searchtype=author&query=Nelan%2C+E+P">E. P. Nelan</a>, <a href="/search/astro-ph?searchtype=author&query=Patterson%2C+R+J">R. J. Patterson</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">A. Sarajedini</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="1702.00803v1-abstract-short" style="display: inline;"> Hubble Space Telescope (HST) fine guidance sensor observations were used to obtain parallaxes of eight metal-poor ([Fe/H] < -1.4) stars. The parallaxes of these stars determined by the revised Hipparcos reduction average 17% accuracy, in contrast to our new HST parallaxes which average 1% accuracy and have errors on the individual parallaxes ranging from 85 to 144 microarcsecond. This parallax dat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1702.00803v1-abstract-full').style.display = 'inline'; document.getElementById('1702.00803v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1702.00803v1-abstract-full" style="display: none;"> Hubble Space Telescope (HST) fine guidance sensor observations were used to obtain parallaxes of eight metal-poor ([Fe/H] < -1.4) stars. The parallaxes of these stars determined by the revised Hipparcos reduction average 17% accuracy, in contrast to our new HST parallaxes which average 1% accuracy and have errors on the individual parallaxes ranging from 85 to 144 microarcsecond. This parallax data has been combined with HST ACS photometry in the F606W and F814W filters to obtain the absolute magnitudes of the stars with an accuracy of 0.02 to 0.03 magnitudes. Six of these stars are on the main sequence (with -2.7 < [Fe/H] < -1.8), and suitable for testing metal-poor stellar evolution models and determining the distances to metal-poor globular clusters. Using the abundances obtained by O'Malley et al. (2017) we find that standard stellar models using the Vandenberg & Clem (2003) color transformation do a reasonable job of matching five of the main sequence stars, with HD 54639 ([Fe/H] = -2.5) being anomalous in its location in the color-magnitude diagram. Stellar models and isochrones were generated using a Monte Carlo analysis to take into account uncertainties in the models. Isochrones which fit the parallax stars were used to determine the distances and ages of nine globular clusters (with -2.4 <= [Fe/H] <= -1.9$). Averaging together the age of all nine clusters, leads to an absolute age of the oldest, most metal-poor globular clusters of 12.7+/- 1.0 Gyr, where the quoted uncertainty takes into account the known uncertainties in the stellar models and isochrones, along with the uncertainty in the distance and reddening of the clusters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1702.00803v1-abstract-full').style.display = 'none'; document.getElementById('1702.00803v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 February, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">37 pages, 10 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/1612.01811">arXiv:1612.01811</a> <span> [<a href="https://arxiv.org/pdf/1612.01811">pdf</a>, <a href="https://arxiv.org/format/1612.01811">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/stw3206">10.1093/mnras/stw3206 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Properties of the Magellanic Bridge Based on OGLE IV RR Lyrae Variables </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wagner-Kaiser%2C+R">R. Wagner-Kaiser</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">Ata Sarajedini</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1612.01811v1-abstract-short" style="display: inline;"> We examine the properties of the Magellanic Bridge connecting the Large and Small Magellanic Clouds using ab-type RR Lyrae variables from the extensive dataset of the Optical Gravitational Lensing Experiment (OGLE), Phase IV data release. The metallicities of the RR Lyraes are determined from the characteristics of their light curves, with an average abundance of [Fe/H] = -1.790 +/- 0.011 (sem) in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1612.01811v1-abstract-full').style.display = 'inline'; document.getElementById('1612.01811v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1612.01811v1-abstract-full" style="display: none;"> We examine the properties of the Magellanic Bridge connecting the Large and Small Magellanic Clouds using ab-type RR Lyrae variables from the extensive dataset of the Optical Gravitational Lensing Experiment (OGLE), Phase IV data release. The metallicities of the RR Lyraes are determined from the characteristics of their light curves, with an average abundance of [Fe/H] = -1.790 +/- 0.011 (sem) in the Magellanic Bridge. From the individual reddenings of these stars, derived via their minimum light curve colors, we determined a median color excess of E(V-I) = 0.101 +/- 0.007 (sem) (implying E(B-V) $\approx$ 0.077). The peak distance modulus of 18.57 +/- 0.048 (sem) places the Bridge stars at distances between the two systems. The metallicity and distance distributions probe the structure of the Magellanic system as a whole, revealing a smooth transition that connects the galaxies. An examination of the HI content does not find a clear correlation between HI emission strength and RR Lyrae spatial distribution, suggesting that the old stellar populations may trace the overlapping halo distributions of the two Magellanic Clouds. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1612.01811v1-abstract-full').style.display = 'none'; document.getElementById('1612.01811v1-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 December, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted 2016 December 5. Received 2016 December 5; in original form 2016 November 7. 10 pages, 8 figures, 5 Tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1612.00714">arXiv:1612.00714</a> <span> [<a href="https://arxiv.org/pdf/1612.00714">pdf</a>, <a href="https://arxiv.org/format/1612.00714">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/10.3847/1538-3881/153/1/19">10.3847/1538-3881/153/1/19 <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. VIII. Preliminary Public Catalog Release </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Soto%2C+M">M. Soto</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">A. Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Piotto%2C+G">G. Piotto</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=van+der+Marel%2C+R+P">R. P. van der Marel</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=Brown%2C+T+M">T. M. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Cool%2C+A+M">A. M. Cool</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=Sarajedini%2C+A">A. Sarajedini</a>, <a href="/search/astro-ph?searchtype=author&query=Granata%2C+V">V. Granata</a>, <a href="/search/astro-ph?searchtype=author&query=Cassisi%2C+S">S. Cassisi</a>, <a href="/search/astro-ph?searchtype=author&query=Aparicio%2C+A">A. Aparicio</a>, <a href="/search/astro-ph?searchtype=author&query=Hidalgo%2C+S">S. Hidalgo</a>, <a href="/search/astro-ph?searchtype=author&query=Ortolani%2C+S">S. Ortolani</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="1612.00714v1-abstract-short" style="display: inline;"> The Hubble Space Telescope (HST) UV Legacy Survey of Galactic Globular Clusters (GO-13297) has been specifically designed to complement the existing F606W and F814W observations of the Advanced Camera for Surveys (ACS) Globular Cluster Survey (GO-10775) by observing the most accessible 47 of the previous survey's 65 clusters in three WFC3/UVIS filters F275W, F336W, and F438W. The new survey also a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1612.00714v1-abstract-full').style.display = 'inline'; document.getElementById('1612.00714v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1612.00714v1-abstract-full" style="display: none;"> The Hubble Space Telescope (HST) UV Legacy Survey of Galactic Globular Clusters (GO-13297) has been specifically designed to complement the existing F606W and F814W observations of the Advanced Camera for Surveys (ACS) Globular Cluster Survey (GO-10775) by observing the most accessible 47 of the previous survey's 65 clusters in three WFC3/UVIS filters F275W, F336W, and F438W. The new survey also adds super-solar metallicity open cluster NGC 6791 to increase the metallicity diversity. The combined survey provides a homogeneous 5-band data set that can be used to pursue a broad range of scientific investigations. In particular, the chosen UV filters allow the identification of multiple stellar populations by targeting the regions of the spectrum that are sensitive to abundance variations in C, N, and O. In order to provide the community with uniform preliminary catalogs, we have devised an automated procedure that performs high-quality photometry on the new UV observations (along with similar observations of seven other programs in the archive). This procedure finds and measures the potential sources on each individual exposure using library point-spread functions and cross-correlates these observations with the original ACS-Survey catalog. The catalog of 57 clusters we publish here will be useful to identify stars in the different stellar populations, in particular for spectroscopic follow-up. Eventually, we will construct a more sophisticated catalog and artificial-star tests based on an optimal reduction of the UV survey data, but the catalogs presented here give the community the chance to make early use of this HST Treasury survey. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1612.00714v1-abstract-full').style.display = 'none'; document.getElementById('1612.00714v1-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 December, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 4 figures. Accepted for publication in AJ. The catalogs from this program can be accessed at http://www.astro.uda.cl/public_release/globularclusters41.html and http://groups.dfa.unipd.it/ESPG/treasury.php</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1610.00451">arXiv:1610.00451</a> <span> [<a href="https://arxiv.org/pdf/1610.00451">pdf</a>, <a href="https://arxiv.org/ps/1610.00451">ps</a>, <a href="https://arxiv.org/format/1610.00451">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/stw2531">10.1093/mnras/stw2531 <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. IX. The Atlas of Multiple Stellar Populations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Milone%2C+A+P">A. P. Milone</a>, <a href="/search/astro-ph?searchtype=author&query=Piotto%2C+G">G. Piotto</a>, <a href="/search/astro-ph?searchtype=author&query=Renzini%2C+A">A. Renzini</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=Bedin%2C+L+R">L. R. Bedin</a>, <a href="/search/astro-ph?searchtype=author&query=Vesperini%2C+E">E. Vesperini</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Antona%2C+F">F. D'Antona</a>, <a href="/search/astro-ph?searchtype=author&query=Nardiello%2C+D">D. Nardiello</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=King%2C+I+R">I. R. King</a>, <a href="/search/astro-ph?searchtype=author&query=Yong%2C+D">D. Yong</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">A. Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Aparicio%2C+A">A. Aparicio</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">B. Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+T+M">T. M. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Cassisi%2C+S">S. Cassisi</a>, <a href="/search/astro-ph?searchtype=author&query=Ortolani%2C+S">S. Ortolani</a>, <a href="/search/astro-ph?searchtype=author&query=Salaris%2C+M">M. Salaris</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+P">R. P. van der Marel</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="1610.00451v1-abstract-short" style="display: inline;"> We use high-precision photometry of red-giant-branch (RGB) stars in 57 Galactic globular clusters (GCs), mostly from the `Hubble Space Telescope (HST) UV Legacy Survey of Galactic globular clusters', to identify and characterize their multiple stellar populations. For each cluster the pseudo two-color diagram (or `chromosome map') is presented, built with a suitable combination of stellar magnitud… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1610.00451v1-abstract-full').style.display = 'inline'; document.getElementById('1610.00451v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1610.00451v1-abstract-full" style="display: none;"> We use high-precision photometry of red-giant-branch (RGB) stars in 57 Galactic globular clusters (GCs), mostly from the `Hubble Space Telescope (HST) UV Legacy Survey of Galactic globular clusters', to identify and characterize their multiple stellar populations. For each cluster the pseudo two-color diagram (or `chromosome map') is presented, built with a suitable combination of stellar magnitudes in the F275W, F336W, F438W and F814W filters that maximizes the separation between multiple populations. In the chromosome map of most GCs (Type I clusters), stars separate in two distinct groups that we identify with the first (1G) and the second generation (2G). This identification is further supported by noticing that 1G stars have primordial (oxygen-rich, sodium-poor) chemical composition, whereas 2G stars are enhanced in sodium and depleted in oxygen. This 1G-2G separation is not possible for a few GCs where the two sequences have apparently merged into an extended, continuous sequence. In some GCs (Type II clusters) the 1G and/or the 2G sequences appear to be split, hence displaying more complex chromosome maps. These clusters exhibit multiple SGBs also in purely optical color-magnitude diagrams, with the fainter SGB joining into a red RGB which is populated by stars with enhanced heavy-element abundance. We measure the RGB width by using appropriate colors and pseudo-colors. When the metallicity dependence is removed, the RGB width correlates with the cluster mass. The fraction of 1G stars ranges from ~8% to ~67% and anticorrelates with the cluster mass, indicating that incidence and complexity of the multiple population phenomenon both increase with cluster mass. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1610.00451v1-abstract-full').style.display = 'none'; document.getElementById('1610.00451v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 October, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 24 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/1609.01527">arXiv:1609.01527</a> <span> [<a href="https://arxiv.org/pdf/1609.01527">pdf</a>, <a href="https://arxiv.org/format/1609.01527">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/stw2247">10.1093/mnras/stw2247 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Bayesian Analysis of Two Stellar Populations in Galactic Globular Clusters III: Analysis of 30 Clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wagner-Kaiser%2C+R">R. Wagner-Kaiser</a>, <a href="/search/astro-ph?searchtype=author&query=Stenning%2C+D+C">D. C. Stenning</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">A. Sarajedini</a>, <a href="/search/astro-ph?searchtype=author&query=von+Hippel%2C+T">T. von Hippel</a>, <a href="/search/astro-ph?searchtype=author&query=van+Dyk%2C+D+A">D. A. van Dyk</a>, <a href="/search/astro-ph?searchtype=author&query=Robinson%2C+E">E. Robinson</a>, <a href="/search/astro-ph?searchtype=author&query=Stein%2C+N">N. Stein</a>, <a href="/search/astro-ph?searchtype=author&query=Jefferys%2C+W+H">W. H. Jefferys</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="1609.01527v1-abstract-short" style="display: inline;"> We use Cycle 21 Hubble Space Telescope (HST) observations and HST archival ACS Treasury observations of 30 Galactic Globular Clusters to characterize two distinct stellar populations. A sophisticated Bayesian technique is employed to simultaneously sample the joint posterior distribution of age, distance, and extinction for each cluster, as well as unique helium values for two populations within e… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.01527v1-abstract-full').style.display = 'inline'; document.getElementById('1609.01527v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1609.01527v1-abstract-full" style="display: none;"> We use Cycle 21 Hubble Space Telescope (HST) observations and HST archival ACS Treasury observations of 30 Galactic Globular Clusters to characterize two distinct stellar populations. A sophisticated Bayesian technique is employed to simultaneously sample the joint posterior distribution of age, distance, and extinction for each cluster, as well as unique helium values for two populations within each cluster and the relative proportion of those populations. We find the helium differences among the two populations in the clusters fall in the range of ~0.04 to 0.11. Because adequate models varying in CNO are not presently available, we view these spreads as upper limits and present them with statistical rather than observational uncertainties. Evidence supports previous studies suggesting an increase in helium content concurrent with increasing mass of the cluster and also find that the proportion of the first population of stars increases with mass as well. Our results are examined in the context of proposed globular cluster formation scenarios. Additionally, we leverage our Bayesian technique to shed light on inconsistencies between the theoretical models and the observed data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.01527v1-abstract-full').style.display = 'none'; document.getElementById('1609.01527v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 September, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 11 figures, 4 tables. Accepted, 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/1605.04827">arXiv:1605.04827</a> <span> [<a href="https://arxiv.org/pdf/1605.04827">pdf</a>, <a href="https://arxiv.org/format/1605.04827">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stw1190">10.1093/mnras/stw1190 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A far-ultraviolet variable with an 18-minute period in the globular cluster NGC 1851 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zurek%2C+D+R">D. R. Zurek</a>, <a href="/search/astro-ph?searchtype=author&query=Knigge%2C+C">C. Knigge</a>, <a href="/search/astro-ph?searchtype=author&query=Maccarone%2C+T+J">T. J. Maccarone</a>, <a href="/search/astro-ph?searchtype=author&query=Pooley%2C+D">D. Pooley</a>, <a href="/search/astro-ph?searchtype=author&query=Dieball%2C+A">A. Dieball</a>, <a href="/search/astro-ph?searchtype=author&query=Long%2C+K+S">K. S. Long</a>, <a href="/search/astro-ph?searchtype=author&query=Shara%2C+M">M. Shara</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">A. Sarajedini</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="1605.04827v2-abstract-short" style="display: inline;"> We present the detection of a variable star with an $18.05$ minute period in far-ultraviolet (FUV) images of the globular cluster NGC 1851 taken with the Hubble Space Telescope (HST). A candidate optical counterpart lies on the red horizontal branch or the asymptotic giant branch star of the cluster, but it is statistically possible that this is a chance superposition. This interpretation is suppo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.04827v2-abstract-full').style.display = 'inline'; document.getElementById('1605.04827v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1605.04827v2-abstract-full" style="display: none;"> We present the detection of a variable star with an $18.05$ minute period in far-ultraviolet (FUV) images of the globular cluster NGC 1851 taken with the Hubble Space Telescope (HST). A candidate optical counterpart lies on the red horizontal branch or the asymptotic giant branch star of the cluster, but it is statistically possible that this is a chance superposition. This interpretation is supported by optical spectroscopt obtained with HST/STIS: the spectrum contains none of the strong emission lines that would be expected if the object was a symbiotic star (i.e. a compact accretor fed by a giant donor). We therefore consider two other possibilities for the nature of FUV variable: (i) an intermediate polar (i.e. a compact binary containing an accreting magnetic white dwarf), or (ii) an AM CVn star (i.e. an interacting double-degenerate system). In the intermediate polar scenario, the object is expected to be an X-ray source. However, no X-rays are detected at its location in $\simeq 65$~ksec of {\em Chandra} imaging, which limits the X-ray luminosity to $L_X \leqslant 10^{32}$~erg~s$^{-1}$. We therefore favour the AM CVn interpretation, but a FUV spectrum is needed to distinguish conclusively between the two possibilities. If the object is an AM CVn binary, it would be the first such system known in any globular cluster. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.04827v2-abstract-full').style.display = 'none'; document.getElementById('1605.04827v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 May, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 May, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 10 figures, Accepted to MNRAS 2016 May 16</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1604.06074">arXiv:1604.06074</a> <span> [<a href="https://arxiv.org/pdf/1604.06074">pdf</a>, <a href="https://arxiv.org/format/1604.06074">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/10.3847/0004-637X/826/1/42">10.3847/0004-637X/826/1/42 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Bayesian Analysis of Two Stellar Populations in Galactic Globular Clusters II: NGC 5024, NGC 5272, and NGC 6352 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wagner-Kaiser%2C+R">R. Wagner-Kaiser</a>, <a href="/search/astro-ph?searchtype=author&query=Stenning%2C+D+C">D. C. Stenning</a>, <a href="/search/astro-ph?searchtype=author&query=Robinson%2C+E">E. Robinson</a>, <a href="/search/astro-ph?searchtype=author&query=von+Hippel%2C+T">T. von Hippel</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">A. Sarajedini</a>, <a href="/search/astro-ph?searchtype=author&query=van+Dyk%2C+D+A">D. A. van Dyk</a>, <a href="/search/astro-ph?searchtype=author&query=Stein%2C+N">N. Stein</a>, <a href="/search/astro-ph?searchtype=author&query=Jefferys%2C+W+H">W. H. Jefferys</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="1604.06074v1-abstract-short" style="display: inline;"> We use Cycle 21 Hubble Space Telescope (HST) observations and HST archival ACS Treasury observations of Galactic Globular Clusters to find and characterize two stellar populations in NGC 5024 (M53), NGC 5272 (M3), and NGC 6352. For these three clusters, both single and double-population analyses are used to determine a best fit isochrone(s). We employ a sophisticated Bayesian analysis technique to… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.06074v1-abstract-full').style.display = 'inline'; document.getElementById('1604.06074v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1604.06074v1-abstract-full" style="display: none;"> We use Cycle 21 Hubble Space Telescope (HST) observations and HST archival ACS Treasury observations of Galactic Globular Clusters to find and characterize two stellar populations in NGC 5024 (M53), NGC 5272 (M3), and NGC 6352. For these three clusters, both single and double-population analyses are used to determine a best fit isochrone(s). We employ a sophisticated Bayesian analysis technique to simultaneously fit the cluster parameters (age, distance, absorption, and metallicity) that characterize each cluster. For the two-population analysis, unique population level helium values are also fit to each distinct population of the cluster and the relative proportions of the populations are determined. We find differences in helium ranging from $\sim$0.05 to 0.11 for these three clusters. Model grids with solar $伪$-element abundances ([$伪$/Fe] =0.0) and enhanced $伪$-elements ([$伪$/Fe]=0.4) are adopted. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.06074v1-abstract-full').style.display = 'none'; document.getElementById('1604.06074v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 April, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">ApJ, 21 pages, 14 figures, 7 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1604.06073">arXiv:1604.06073</a> <span> [<a href="https://arxiv.org/pdf/1604.06073">pdf</a>, <a href="https://arxiv.org/format/1604.06073">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/10.3847/0004-637X/826/1/41">10.3847/0004-637X/826/1/41 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Bayesian Analysis of Two Stellar Populations in Galactic Globular Clusters I: Statistical and Computational Methods </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Stenning%2C+D+C">D. C. Stenning</a>, <a href="/search/astro-ph?searchtype=author&query=Wagner-Kaiser%2C+R">R. Wagner-Kaiser</a>, <a href="/search/astro-ph?searchtype=author&query=Robinson%2C+E">E. Robinson</a>, <a href="/search/astro-ph?searchtype=author&query=van+Dyk%2C+D+A">D. A. van Dyk</a>, <a href="/search/astro-ph?searchtype=author&query=von+Hippel%2C+T">T. von Hippel</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">A. Sarajedini</a>, <a href="/search/astro-ph?searchtype=author&query=Stein%2C+N">N. Stein</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="1604.06073v2-abstract-short" style="display: inline;"> We develop a Bayesian model for globular clusters composed of multiple stellar populations, extending earlier statistical models for open clusters composed of simple (single) stellar populations (vanDyk et al. 2009, Stein et al. 2013). Specifically, we model globular clusters with two populations that differ in helium abundance. Our model assumes a hierarchical structuring of the parameters in whi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.06073v2-abstract-full').style.display = 'inline'; document.getElementById('1604.06073v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1604.06073v2-abstract-full" style="display: none;"> We develop a Bayesian model for globular clusters composed of multiple stellar populations, extending earlier statistical models for open clusters composed of simple (single) stellar populations (vanDyk et al. 2009, Stein et al. 2013). Specifically, we model globular clusters with two populations that differ in helium abundance. Our model assumes a hierarchical structuring of the parameters in which physical properties---age, metallicity, helium abundance, distance, absorption, and initial mass---are common to (i) the cluster as a whole or to (ii) individual populations within a cluster, or are unique to (iii) individual stars. An adaptive Markov chain Monte Carlo (MCMC) algorithm is devised for model fitting that greatly improves convergence relative to its precursor non-adaptive MCMC algorithm. Our model and computational tools are incorporated into an open-source software suite known as BASE-9. We use numerical studies to demonstrate that our method can recover parameters of two-population clusters, and also show model misspecification can potentially be identified. As a proof of concept, we analyze the two stellar populations of globular cluster NGC 5272 using our model and methods. (BASE-9 is available from GitHub: https://github.com/argiopetech/base/releases). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.06073v2-abstract-full').style.display = 'none'; document.getElementById('1604.06073v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 April, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 April, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 9 figures, 2 tables. To be published in The Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1603.07651">arXiv:1603.07651</a> <span> [<a href="https://arxiv.org/pdf/1603.07651">pdf</a>, <a href="https://arxiv.org/format/1603.07651">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/10.3847/0004-637X/822/1/44">10.3847/0004-637X/822/1/44 <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. VII. Implications from the Nearly Universal Nature of Horizontal Branch Discontinuities </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Brown%2C+T+M">Thomas M. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Cassisi%2C+S">Santi Cassisi</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Antona%2C+F">Francesca D'Antona</a>, <a href="/search/astro-ph?searchtype=author&query=Salaris%2C+M">Maurizio Salaris</a>, <a href="/search/astro-ph?searchtype=author&query=Milone%2C+A+P">Antonino P. Milone</a>, <a href="/search/astro-ph?searchtype=author&query=Dalessandro%2C+E">Emanuele Dalessandro</a>, <a href="/search/astro-ph?searchtype=author&query=Piotto%2C+G">Giampaolo Piotto</a>, <a href="/search/astro-ph?searchtype=author&query=Renzini%2C+A">Alvio Renzini</a>, <a href="/search/astro-ph?searchtype=author&query=Sweigart%2C+A+V">Allen V. Sweigart</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">Andrea Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Ortolani%2C+S">Sergio Ortolani</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">Ata Sarajedini</a>, <a href="/search/astro-ph?searchtype=author&query=Aparicio%2C+A">Antonio Aparicio</a>, <a href="/search/astro-ph?searchtype=author&query=Bedin%2C+L+R">Luigi R. Bedin</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">Jay Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Pietrinferni%2C+A">Adriano Pietrinferni</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="1603.07651v1-abstract-short" style="display: inline;"> The UV-initiative Hubble Space Telescope Treasury survey of Galactic globular clusters provides a new window into the phenomena that shape the morphological features of the horizontal branch (HB). Using this large and homogeneous catalog of UV and blue photometry, we demonstrate that the HB exhibits discontinuities that are remarkably consistent in color (effective temperature). This consistency i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1603.07651v1-abstract-full').style.display = 'inline'; document.getElementById('1603.07651v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1603.07651v1-abstract-full" style="display: none;"> The UV-initiative Hubble Space Telescope Treasury survey of Galactic globular clusters provides a new window into the phenomena that shape the morphological features of the horizontal branch (HB). Using this large and homogeneous catalog of UV and blue photometry, we demonstrate that the HB exhibits discontinuities that are remarkably consistent in color (effective temperature). This consistency is apparent even among some of the most massive clusters hosting multiple distinct sub-populations (such as NGC 2808, omega Cen, and NGC 6715), demonstrating that these phenomena are primarily driven by atmospheric physics that is independent of the underlying population properties. However, inconsistencies arise in the metal-rich clusters NGC 6388 and NGC 6441, where the discontinuity within the blue HB (BHB) distribution shifts ~1,000 K to 2,000 K hotter. We demonstrate that this shift is likely due to a large helium enhancement in the BHB stars of these clusters, which in turn affects the surface convection and evolution of such stars. Our survey also increases the number of Galactic globular clusters known to host blue-hook stars (also known as late hot flashers) from 6 to 23 clusters. These clusters are biased toward the bright end of the globular cluster luminosity function, confirming that blue-hook stars tend to form in the most massive clusters with significant self-enrichment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1603.07651v1-abstract-full').style.display = 'none'; document.getElementById('1603.07651v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 March, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in The Astrophysical Journal. 21 pages, 9 color figures, 1 table</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1510.07075">arXiv:1510.07075</a> <span> [<a href="https://arxiv.org/pdf/1510.07075">pdf</a>, <a href="https://arxiv.org/format/1510.07075">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The pulsating variable star population in DDO210 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ordo%C3%B1ez%2C+A+J">Antonio J. Ordo帽ez</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">Ata Sarajedini</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="1510.07075v1-abstract-short" style="display: inline;"> We have probed the pulsating variable star content of the isolated Local Group dwarf galaxy, DDO210 (Aquarius), using archival Advanced Camera for Surveys/$Hubble$ $Space$ $Telescope$ imaging in the F475W and F814W passbands. We find a total of 32 RR Lyrae stars (24 ab-type, 8 c-type) and 75 Cepheid variables. The mean periods of the ab-type and c-type RR Lyrae stars are calculated to be… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1510.07075v1-abstract-full').style.display = 'inline'; document.getElementById('1510.07075v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1510.07075v1-abstract-full" style="display: none;"> We have probed the pulsating variable star content of the isolated Local Group dwarf galaxy, DDO210 (Aquarius), using archival Advanced Camera for Surveys/$Hubble$ $Space$ $Telescope$ imaging in the F475W and F814W passbands. We find a total of 32 RR Lyrae stars (24 ab-type, 8 c-type) and 75 Cepheid variables. The mean periods of the ab-type and c-type RR Lyrae stars are calculated to be $\langle$P$_{\mathrm{ab}}\rangle = 0.609\pm0.011$ and $\langle$P$_{\mathrm{c}}\rangle = 0.359\pm0.025$ days, respectively. The light curve properties of the fundamental mode RR Lyrae stars yield a mean metallicity of $\langle$[Fe/H]$\rangle$ = -1.63$\pm$0.11 dex for this ancient population, consistent with a recent synthetic colour-magnitude diagram analysis. We find this galaxy to be Oosterhoff-intermediate and lacking in high-amplitude, short-period ab-type RR Lyrae, consistent with behavior recently observed for many dwarf spheroidals and ultra-faint dwarfs in the Local Group. We find a distance modulus of $渭= 25.07\pm 0.12$ as determined by the RR Lyrae stars, slightly larger but agreeing with recent distance estimates from the red giant branch tip. We also find a sizable population of Cepheid variables in this galaxy. We provide evidence in favor of most if not all of these stars being short-period classical Cepheids. Assuming all of these stars to be classical Cepheids, we find that most of these Cepheids are $\sim$300 Myr old, with the youngest Cepheids being offset from the older Cepheids and the centre of the galaxy. We conclude that this may have resulted from a migration of star formation in DDO210. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1510.07075v1-abstract-full').style.display = 'none'; document.getElementById('1510.07075v1-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 October, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication into MNRAS, 17 pages, 13 figures, 4 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1510.03682">arXiv:1510.03682</a> <span> [<a href="https://arxiv.org/pdf/1510.03682">pdf</a>, <a href="https://arxiv.org/ps/1510.03682">ps</a>, <a href="https://arxiv.org/format/1510.03682">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/10.3847/0004-6256/151/4/88">10.3847/0004-6256/151/4/88 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Large Magellanic Cloud Near-Infrared Synoptic Survey. II. The Wesenheit relations and their application to the Distance scale </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bhardwaj%2C+A">Anupam Bhardwaj</a>, <a href="/search/astro-ph?searchtype=author&query=Kanbur%2C+S+M">Shashi M. Kanbur</a>, <a href="/search/astro-ph?searchtype=author&query=Macri%2C+L+M">Lucas M. Macri</a>, <a href="/search/astro-ph?searchtype=author&query=Singh%2C+H+P">Harinder P. Singh</a>, <a href="/search/astro-ph?searchtype=author&query=Ngeow%2C+C">Chow-Choong Ngeow</a>, <a href="/search/astro-ph?searchtype=author&query=Wagner-Kaiser%2C+R">R. Wagner-Kaiser</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">Ata Sarajedini</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="1510.03682v1-abstract-short" style="display: inline;"> We present new near-infrared Cepheid Period-Wesenheit relations in the LMC using time-series observations from the Large Magellanic Cloud Near-Infrared Synoptic Survey. We also derive optical$+$near-infrared P-W relations using $V$ and $I$~magnitudes from OGLE-III. We employ our new $JHK_s$ data to determine an independent distance to the LMC of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1510.03682v1-abstract-full').style.display = 'inline'; document.getElementById('1510.03682v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1510.03682v1-abstract-full" style="display: none;"> We present new near-infrared Cepheid Period-Wesenheit relations in the LMC using time-series observations from the Large Magellanic Cloud Near-Infrared Synoptic Survey. We also derive optical$+$near-infrared P-W relations using $V$ and $I$~magnitudes from OGLE-III. We employ our new $JHK_s$ data to determine an independent distance to the LMC of $渭_{\rm LMC} = 18.47\pm0.07 {\textit{(statistical)}}$~mag, using an absolute calibration of the Galactic relations based on several distance determination methods and accounting for the intrinsic scatter of each technique. We also derive new near-infrared Period-Luminosity and Wesenheit relations for Cepheids in M31 using observations from the PHAT survey. We use the absolute calibrations of the Galactic and LMC $W_{J,H}$ relations to determine the distance modulus of M31, $渭_{\rm M31} = 24.46\pm0.20$~mag. We apply a simultaneous fit to Cepheids in several Local Group galaxies covering a range of metallicities ($7.7<12+\log[O/H]<8.6$~dex) to determine a global slope of -$3.244\pm0.016$~mag/dex for the $W_{J,K_s}$ relation and obtain robust distance estimates. Our distances are in good agreement with recent TRGB based distance estimates and we do not find any evidence for a metallicity dependence in the near-infrared P-W relations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1510.03682v1-abstract-full').style.display = 'none'; document.getElementById('1510.03682v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 October, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 8 figures, Accepted for publication in The Astronomical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1510.01468">arXiv:1510.01468</a> <span> [<a href="https://arxiv.org/pdf/1510.01468">pdf</a>, <a href="https://arxiv.org/ps/1510.01468">ps</a>, <a href="https://arxiv.org/format/1510.01468">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/stv2268">10.1093/mnras/stv2268 <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. V. Constraints on Formation Scenarios </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Renzini%2C+A">A. Renzini</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=Cassisi%2C+S">S. Cassisi</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=Milone%2C+A+P">A. P. Milone</a>, <a href="/search/astro-ph?searchtype=author&query=Ventura%2C+P">P. Ventura</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">J. Anderson</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=Bellini%2C+A">A. Bellini</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=Piotto%2C+G">G. Piotto</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Marel%2C+R+P">R. P. van der Marel</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">B. Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=Dalessandro%2C+E">E. Dalessandro</a>, <a href="/search/astro-ph?searchtype=author&query=Hidalgo%2C+S">S. Hidalgo</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=Ortolani%2C+S">S. Ortolani</a>, <a href="/search/astro-ph?searchtype=author&query=Salaris%2C+M">M. Salaris</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">A. Sarajedini</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="1510.01468v1-abstract-short" style="display: inline;"> We build on the evidence provided by our Legacy Survey of Galactic globular clusters (GC) to submit to a crucial test four scenarios currently entertained for the formation of multiple stellar generations in GCs. The observational constraints on multiple generations to be fulfilled are manifold, including GC specificity, ubiquity, variety, predominance, discreteness, supernova avoidance, p-capture… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1510.01468v1-abstract-full').style.display = 'inline'; document.getElementById('1510.01468v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1510.01468v1-abstract-full" style="display: none;"> We build on the evidence provided by our Legacy Survey of Galactic globular clusters (GC) to submit to a crucial test four scenarios currently entertained for the formation of multiple stellar generations in GCs. The observational constraints on multiple generations to be fulfilled are manifold, including GC specificity, ubiquity, variety, predominance, discreteness, supernova avoidance, p-capture processing, helium enrichment and mass budget. We argue that scenarios appealing to supermassive stars, fast rotating massive stars and massive interactive binaries violate in an irreparable fashion two or more among such constraints. Also the scenario appealing to AGB stars as producers of the material for next generation stars encounters severe difficulties, specifically concerning the mass budget problem and the detailed chemical composition of second generation stars. We qualitatively explore ways possibly allowing one to save the AGB scenario, specifically appealing to a possible revision of the cross section of a critical reaction rate destroying sodium, or alternatively by a more extensive exploration of the vast parameter space controlling the evolutionary behavior of AGB stellar models. Still, we cannot ensure success for these efforts and totally new scenarios may have to be invented to understand how GCs formed in the early Universe. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1510.01468v1-abstract-full').style.display = 'none'; document.getElementById('1510.01468v1-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 October, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 3 figures, to appear on Monthly Notices of the Royal Astronomical Society</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1504.06128">arXiv:1504.06128</a> <span> [<a href="https://arxiv.org/pdf/1504.06128">pdf</a>, <a href="https://arxiv.org/ps/1504.06128">ps</a>, <a href="https://arxiv.org/format/1504.06128">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Evidence for temporal evolution in the M33 disc as traced by its star clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Beasley%2C+M+A">Michael A. Beasley</a>, <a href="/search/astro-ph?searchtype=author&query=Roman%2C+I+S">Izaskun San Roman</a>, <a href="/search/astro-ph?searchtype=author&query=Gallart%2C+C">Carme Gallart</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">Ata Sarajedini</a>, <a href="/search/astro-ph?searchtype=author&query=Aparicio%2C+A">Antonio Aparicio</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="1504.06128v1-abstract-short" style="display: inline;"> We present precision radial velocities and stellar population parameters for 77 star clusters in the Local Group galaxy M33. Our GTC and WHT observations sample both young, massive clusters and known/candidate globular clusters, spanning ages ~ 10^6 - 10^10 yr, and metallicities, [M/H] ~-1.7 to solar. The cluster system exhibits an age-metallicity relation; the youngest clusters are the most metal… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1504.06128v1-abstract-full').style.display = 'inline'; document.getElementById('1504.06128v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1504.06128v1-abstract-full" style="display: none;"> We present precision radial velocities and stellar population parameters for 77 star clusters in the Local Group galaxy M33. Our GTC and WHT observations sample both young, massive clusters and known/candidate globular clusters, spanning ages ~ 10^6 - 10^10 yr, and metallicities, [M/H] ~-1.7 to solar. The cluster system exhibits an age-metallicity relation; the youngest clusters are the most metal-rich. When compared to HI data, clusters with [M/H] ~ -1.0 and younger than ~ 4 Gyr are clearly identified as a disc population. The clusters show evidence for strong time evolution in the disc radial metallicity gradient (d[M/H]dt / dR = 0.03 dex/kpc/Gyr). The oldest clusters have stronger, more negative gradients than the youngest clusters in M33. The clusters also show a clear age-velocity dispersion relation. The line of sight velocity dispersions of the clusters increases with age similar to Milky Way open clusters and stars. The general shape of the relation is reproduced by disc heating simulations, and the similarity between the relations in M33 and the Milky Way suggests that heating by substructure, and cooling of the ISM both play a role in shaping this relation. We identify 12 "classical" GCs, six of which are newly identified GC candidates. The GCs are more metal-rich than Milky Way halo clusters, and show weak rotation. The inner (R < 4.5 kpc) GCs exhibit a steep radial metallicity gradient (d[M/H]/dR = -0.29+-0.11 dex/kpc) and an exponential-like surface density profile. We argue that these inner GCs are thick disc rather than halo objects. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1504.06128v1-abstract-full').style.display = 'none'; document.getElementById('1504.06128v1-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 April, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">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/1504.05118">arXiv:1504.05118</a> <span> [<a href="https://arxiv.org/pdf/1504.05118">pdf</a>, <a href="https://arxiv.org/format/1504.05118">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/stv880">10.1093/mnras/stv880 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Panchromatic Hubble Andromeda Treasury XIII: The Cepheid period-luminosity relation in M31 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wagner-Kaiser%2C+R">R. Wagner-Kaiser</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">A. Sarajedini</a>, <a href="/search/astro-ph?searchtype=author&query=Dalcanton%2C+J+J">J. J. Dalcanton</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+B+F">B. F. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A">A. Dolphin</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="1504.05118v2-abstract-short" style="display: inline;"> Using Hubble Space Telescope Advanced Camera for Surveys (HST/ACS) and Wide Field Camera 3 (WFC3) observations from the Panchromatic Hubble Andromeda Treasury (PHAT), we present new period-luminosity (P-L) relations for Cepheid variables in M31. Cepheids from several ground-based studies are identified in the PHAT photometry to derive new P-L and Wesenheit P-L relations in the near infrared and vi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1504.05118v2-abstract-full').style.display = 'inline'; document.getElementById('1504.05118v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1504.05118v2-abstract-full" style="display: none;"> Using Hubble Space Telescope Advanced Camera for Surveys (HST/ACS) and Wide Field Camera 3 (WFC3) observations from the Panchromatic Hubble Andromeda Treasury (PHAT), we present new period-luminosity (P-L) relations for Cepheid variables in M31. Cepheids from several ground-based studies are identified in the PHAT photometry to derive new P-L and Wesenheit P-L relations in the near infrared and visual filters. We derive a distance modulus to M31 of 24.51 +/- 0.08 in the IR bands and 24.32 +/- 0.09 in the visual bands, including the first P-L relations in the F475W and F814W filters for M31. Our derived visual and IR distance moduli disagree at slightly more than a 1蟽 level. Differences in the P-L relations between ground-based and HST observations are investigated for a subset of Cepheids. We find a significant discrepancy between ground-based and HST P-L relations with the same Cepheids, suggesting adverse effects from photometric contamination in ground-based Cepheid observations. Additionally, a statistically significant radial trend in the P-L relation is found which does not appear to be explained by metallicity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1504.05118v2-abstract-full').style.display = 'none'; document.getElementById('1504.05118v2-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 July, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 April, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 15 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/1504.00909">arXiv:1504.00909</a> <span> [<a href="https://arxiv.org/pdf/1504.00909">pdf</a>, <a href="https://arxiv.org/format/1504.00909">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-6256/149/6/201">10.1088/0004-6256/149/6/201 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Population Effects on the Metallicity Distribution Function Derived From the Red Giant Branch </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ordo%C3%B1ez%2C+A+J">Antonio J. Ordo帽ez</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">Ata Sarajedini</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="1504.00909v2-abstract-short" style="display: inline;"> We have tested the reliability of the red giant branch (RGB) as a metallicity indicator accounting for observational errors as well as the complexity of star formation histories (SFHs) and chemical evolution histories observed in various stellar systems. We generate model color-magnitude diagrams (CMDs) produced with a variety of evolutionary histories and compare the resultant metallicity estimat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1504.00909v2-abstract-full').style.display = 'inline'; document.getElementById('1504.00909v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1504.00909v2-abstract-full" style="display: none;"> We have tested the reliability of the red giant branch (RGB) as a metallicity indicator accounting for observational errors as well as the complexity of star formation histories (SFHs) and chemical evolution histories observed in various stellar systems. We generate model color-magnitude diagrams (CMDs) produced with a variety of evolutionary histories and compare the resultant metallicity estimates from the colors and magnitudes of RGB stars to the true input metallicities. We include realistic models for photometric errors and completeness in our synthetic CMDs. As expected, for simple simple stellar populations dominated by old stars, the RGB provides a very accurate estimate of the modular metallicity value for a population. An error in the age of a system targeted for this type of study may produce metallicity errors of a few tenths of a dex. The size of this metallicity error depends linearly on the age error, and we find this dependence to be stronger with more precise photometry. If the population has experienced any significant star formation within the last $\sim$6 Gyr, the metallicity estimates, [M/H], derived from the RGB may be in error by up to $\sim$0.5 dex. Perhaps the most important consideration for this technique is an accurate, independent estimate of the average age for the target stellar system, especially if it is probable that a significant fraction of the population formed less than $\sim$6 Gyr ago. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1504.00909v2-abstract-full').style.display = 'none'; document.getElementById('1504.00909v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 April, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 April, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1503.02909">arXiv:1503.02909</a> <span> [<a href="https://arxiv.org/pdf/1503.02909">pdf</a>, <a href="https://arxiv.org/ps/1503.02909">ps</a>, <a href="https://arxiv.org/format/1503.02909">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/10.1088/0004-6256/149/5/154">10.1088/0004-6256/149/5/154 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Ca II Triplet Spectroscopy of Small Magellanic Cloud Red Giants. III. Abundances and Velocities for a Sample of 14 Clusters </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=Geisler%2C+D">D. Geisler</a>, <a href="/search/astro-ph?searchtype=author&query=Clari%C3%A1%2C+J+J">J. J. Clari谩</a>, <a href="/search/astro-ph?searchtype=author&query=Villanova%2C+S">S. Villanova</a>, <a href="/search/astro-ph?searchtype=author&query=Marcionni%2C+N">N. Marcionni</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">A. Sarajedini</a>, <a href="/search/astro-ph?searchtype=author&query=Grocholski%2C+A+J">A. J. Grocholski</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="1503.02909v1-abstract-short" style="display: inline;"> We obtained spectra of red giants in 15 Small Magellanic Cloud (SMC) clusters in the region of the CaII lines with FORS2 on the Very Large Telescope (VLT). We determined the mean metallicity and radial velocity with mean errors of 0.05 dex and 2.6 km/s, respectively, from a mean of 6.5 members per cluster. One cluster (B113) was too young for a reliable metallicity determination and was excluded f… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.02909v1-abstract-full').style.display = 'inline'; document.getElementById('1503.02909v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1503.02909v1-abstract-full" style="display: none;"> We obtained spectra of red giants in 15 Small Magellanic Cloud (SMC) clusters in the region of the CaII lines with FORS2 on the Very Large Telescope (VLT). We determined the mean metallicity and radial velocity with mean errors of 0.05 dex and 2.6 km/s, respectively, from a mean of 6.5 members per cluster. One cluster (B113) was too young for a reliable metallicity determination and was excluded from the sample. We combined the sample studied here with 15 clusters previously studied by us using the same technique, and with 7 clusters whose metallicities determined by other authors are on a scale similar to ours. This compilation of 36 clusters is the largest SMC cluster sample currently available with accurate and homogeneously determined metallicities. We found a high probability that the metallicity distribution is bimodal, with potential peaks at -1.1 and -0.8 dex. Our data show no strong evidence of a metallicity gradient in the SMC clusters, somewhat at odds with recent evidence from CaT spectra of a large sample of field stars Dobbie et al. (2014). This may be revealing possible differences in the chemical history of clusters and field stars. Our clusters show a significant dispersion of metallicities, whatever age is considered, which could be reflecting the lack of a unique AMR in this galaxy. None of the chemical evolution models currently available in the literature satisfactorily represents the global chemical enrichment processes of SMC clusters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.02909v1-abstract-full').style.display = 'none'; document.getElementById('1503.02909v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 March, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">49 pages, 15 figures. Accepted for publication in AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1501.04966">arXiv:1501.04966</a> <span> [<a href="https://arxiv.org/pdf/1501.04966">pdf</a>, <a href="https://arxiv.org/format/1501.04966">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/802/2/127">10.1088/0004-637X/802/2/127 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> PHAT Stellar Cluster Survey. II. Andromeda Project Cluster Catalog </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+L+C">L. Clifton Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Seth%2C+A+C">Anil C. Seth</a>, <a href="/search/astro-ph?searchtype=author&query=Dalcanton%2C+J+J">Julianne J. Dalcanton</a>, <a href="/search/astro-ph?searchtype=author&query=Wallace%2C+M+L">Matthew L. Wallace</a>, <a href="/search/astro-ph?searchtype=author&query=Simpson%2C+R+J">Robert J. Simpson</a>, <a href="/search/astro-ph?searchtype=author&query=Lintott%2C+C+J">Chris J. Lintott</a>, <a href="/search/astro-ph?searchtype=author&query=Kapadia%2C+A">Amit Kapadia</a>, <a href="/search/astro-ph?searchtype=author&query=Skillman%2C+E+D">Evan D. Skillman</a>, <a href="/search/astro-ph?searchtype=author&query=Caldwell%2C+N">Nelson Caldwell</a>, <a href="/search/astro-ph?searchtype=author&query=Fouesneau%2C+M">Morgan Fouesneau</a>, <a href="/search/astro-ph?searchtype=author&query=Weisz%2C+D+R">Daniel R. Weisz</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+B+F">Benjamin F. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Beerman%2C+L+C">Lori C. Beerman</a>, <a href="/search/astro-ph?searchtype=author&query=Gouliermis%2C+D+A">Dimitrios A. Gouliermis</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">Ata Sarajedini</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="1501.04966v1-abstract-short" style="display: inline;"> We construct a stellar cluster catalog for the Panchromatic Hubble Andromeda Treasury (PHAT) survey using image classifications collected from the Andromeda Project citizen science website. We identify 2,753 clusters and 2,270 background galaxies within ~0.5 deg$^2$ of PHAT imaging searched, or ~400 kpc$^2$ in deprojected area at the distance of the Andromeda galaxy (M31). These identifications re… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1501.04966v1-abstract-full').style.display = 'inline'; document.getElementById('1501.04966v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1501.04966v1-abstract-full" style="display: none;"> We construct a stellar cluster catalog for the Panchromatic Hubble Andromeda Treasury (PHAT) survey using image classifications collected from the Andromeda Project citizen science website. We identify 2,753 clusters and 2,270 background galaxies within ~0.5 deg$^2$ of PHAT imaging searched, or ~400 kpc$^2$ in deprojected area at the distance of the Andromeda galaxy (M31). These identifications result from 1.82 million classifications of ~20,000 individual images (totaling ~7 gigapixels) by tens of thousands of volunteers. We show that our crowd-sourced approach, which collects >80 classifications per image, provides a robust, repeatable method of cluster identification. The high spatial resolution Hubble Space Telescope images resolve individual stars in each cluster and are instrumental in the factor of ~6 increase in the number of clusters known within the survey footprint. We measure integrated photometry in six filter passbands, ranging from the near-UV to the near-IR. PHAT clusters span a range of ~8 magnitudes in F475W (g-band) luminosity, equivalent to ~4 decades in cluster mass. We perform catalog completeness analysis using >3000 synthetic cluster simulations to determine robust detection limits and demonstrate that the catalog is 50% complete down to ~500 solar masses for ages <100 Myr. We include catalogs of clusters, background galaxies, remaining unselected candidates, and synthetic cluster simulations, making all information publicly available to the community. The catalog published here serves as the definitive base data product for PHAT cluster science, providing a census of star clusters in an L$^*$ spiral galaxy with unmatched sensitivity and quality. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1501.04966v1-abstract-full').style.display = 'none'; document.getElementById('1501.04966v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 January, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 20 figures, Accepted by ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1411.5043">arXiv:1411.5043</a> <span> [<a href="https://arxiv.org/pdf/1411.5043">pdf</a>, <a href="https://arxiv.org/ps/1411.5043">ps</a>, <a href="https://arxiv.org/format/1411.5043">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stu2446">10.1093/mnras/stu2446 <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. II. The seven stellar populations of NGC7089 (M2) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Milone%2C+A+P">A. P. Milone</a>, <a href="/search/astro-ph?searchtype=author&query=Marino%2C+A+F">A. F. Marino</a>, <a href="/search/astro-ph?searchtype=author&query=Piotto%2C+G">G. Piotto</a>, <a href="/search/astro-ph?searchtype=author&query=Bedin%2C+L+R">L. R. Bedin</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Renzini%2C+A">A. Renzini</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=Bellini%2C+A">A. Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+T+M">T. M. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Cassisi%2C+S">S. Cassisi</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Antona%2C+F">F. D'Antona</a>, <a href="/search/astro-ph?searchtype=author&query=Jerjen%2C+H">H. Jerjen</a>, <a href="/search/astro-ph?searchtype=author&query=Nardiello%2C+D">D. Nardiello</a>, <a href="/search/astro-ph?searchtype=author&query=Salaris%2C+M">M. Salaris</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Marel%2C+R+P">R. P. van der Marel</a>, <a href="/search/astro-ph?searchtype=author&query=Vesperini%2C+E">E. Vesperini</a>, <a href="/search/astro-ph?searchtype=author&query=Yong%2C+D">D. Yong</a>, <a href="/search/astro-ph?searchtype=author&query=Aparicio%2C+A">A. Aparicio</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">A. Sarajedini</a>, <a href="/search/astro-ph?searchtype=author&query=Zoccali%2C+M">M. Zoccali</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="1411.5043v1-abstract-short" style="display: inline;"> We present high-precision multi-band photometry for the globular cluster (GC) M2. We combine the analysis of the photometric data obtained from the Hubble Space Telescope UV Legacy Survey of Galactic GCs GO-13297, with chemical abundances by Yong et al.(2014), and compare the photometry with models in order to analyze the multiple stellar sequences we identified in the color-magnitude diagram (CMD… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1411.5043v1-abstract-full').style.display = 'inline'; document.getElementById('1411.5043v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1411.5043v1-abstract-full" style="display: none;"> We present high-precision multi-band photometry for the globular cluster (GC) M2. We combine the analysis of the photometric data obtained from the Hubble Space Telescope UV Legacy Survey of Galactic GCs GO-13297, with chemical abundances by Yong et al.(2014), and compare the photometry with models in order to analyze the multiple stellar sequences we identified in the color-magnitude diagram (CMD). We find three main stellar components, composed of metal-poor, metal-intermediate, and metal-rich stars (hereafter referred to as population A, B, and C, respectively). The components A and B include stars with different $s$-process element abundances. They host six sub-populations with different light-element abundances, and exhibit an internal variation in helium up to Delta Y~0.07 dex. In contrast with M22, another cluster characterized by the presence of populations with different metallicities, M2 contains a third stellar component, C, which shows neither evidence for sub-populations nor an internal spread in light-elements. Population C does not exhibit the typical photometric signatures that are associated with abundance variations of light elements produced by hydrogen burning at hot temperatures. We compare M2 with other GCs with intrinsic heavy-element variations and conclude that M2 resembles M22, but it includes an additional stellar component that makes it more similar to the central region of the Sagittarius galaxy, which hosts a GC (M54) and the nucleus of the Sagittarius galaxy itself. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1411.5043v1-abstract-full').style.display = 'none'; document.getElementById('1411.5043v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 November, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 7 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/1410.4564">arXiv:1410.4564</a> <span> [<a href="https://arxiv.org/pdf/1410.4564">pdf</a>, <a href="https://arxiv.org/ps/1410.4564">ps</a>, <a href="https://arxiv.org/format/1410.4564">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/10.1088/0004-6256/149/3/91">10.1088/0004-6256/149/3/91 <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. I. Overview of the Project and Detection of Multiple Stellar Populations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Piotto%2C+G">G. Piotto</a>, <a href="/search/astro-ph?searchtype=author&query=Milone%2C+A+P">A. P. Milone</a>, <a href="/search/astro-ph?searchtype=author&query=Bedin%2C+L+R">L. R. Bedin</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=King%2C+I+R">I. R. King</a>, <a href="/search/astro-ph?searchtype=author&query=Marino%2C+A">A. Marino</a>, <a href="/search/astro-ph?searchtype=author&query=Nardiello%2C+D">D. Nardiello</a>, <a href="/search/astro-ph?searchtype=author&query=Aparicio%2C+A">A. Aparicio</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">B. Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">A. Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+T+M">T. M. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Cassisi%2C+S">S. Cassisi</a>, <a href="/search/astro-ph?searchtype=author&query=Cunial%2C+A">A. Cunial</a>, <a href="/search/astro-ph?searchtype=author&query=Dalessandro%2C+E">E. Dalessandro</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=Ferraro%2C+F+R">F. R. Ferraro</a>, <a href="/search/astro-ph?searchtype=author&query=Hidalgo%2C+S">S. Hidalgo</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzoni%2C+B">B. Lanzoni</a>, <a href="/search/astro-ph?searchtype=author&query=Monelli%2C+M">M. Monelli</a>, <a href="/search/astro-ph?searchtype=author&query=Ortolani%2C+S">S. Ortolani</a>, <a href="/search/astro-ph?searchtype=author&query=Renzini%2C+A">A. Renzini</a>, <a href="/search/astro-ph?searchtype=author&query=Salaris%2C+M">M. Salaris</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+P">R. P. van der Marel</a>, <a href="/search/astro-ph?searchtype=author&query=Vesperini%2C+E">E. Vesperini</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="1410.4564v1-abstract-short" style="display: inline;"> In this paper we describe a new UV-initiative HST project (GO-13297) that will complement the existing F606W and F814W database of the ACS Globular Cluster (GC) Treasury by imaging most of its clusters through UV/blue WFC3/UVIS filters F275W, F336W and F438W. This "magic trio" of filters has shown an uncanny ability to disentangle and characterize multiple-population (MP) patterns in GCs in a way… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1410.4564v1-abstract-full').style.display = 'inline'; document.getElementById('1410.4564v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1410.4564v1-abstract-full" style="display: none;"> In this paper we describe a new UV-initiative HST project (GO-13297) that will complement the existing F606W and F814W database of the ACS Globular Cluster (GC) Treasury by imaging most of its clusters through UV/blue WFC3/UVIS filters F275W, F336W and F438W. This "magic trio" of filters has shown an uncanny ability to disentangle and characterize multiple-population (MP) patterns in GCs in a way that is exquisitely sensitive to C, N, and O abundance variations. Combination of these passbands with those in the optical also gives the best leverage for measuring helium enrichment. The dozen clusters that had previously been observed in these bands exhibit a bewildering variety of MP patterns, and the new survey will map the full variance of the phenomenon. The ubiquity of multiple stellar generations in GCs has made the formation of these cornerstone objects more intriguing than ever; GC formation and the origin of their MPs have now become one and the same problem. In the present paper we will describe the data base and our data reduction strategy, as well as the uses we intend to make of the final photometry, astrometry, and proper motions. We will also present preliminary color-magnitude diagrams from the data so far collected. These diagrams also draw on data from GO-12605 and GO-12311, which served as a pilot project for the present GO-13297. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1410.4564v1-abstract-full').style.display = 'none'; document.getElementById('1410.4564v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 October, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">56 pages, 23 figures, 1 table, accepted for publication on AJ. The official TREASURY webpage can be found at this url: http://groups.dfa.unipd.it/ESPG/treasury.html</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1408.1684">arXiv:1408.1684</a> <span> [<a href="https://arxiv.org/pdf/1408.1684">pdf</a>, <a href="https://arxiv.org/format/1408.1684">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/10.1088/0004-6256/148/5/85">10.1088/0004-6256/148/5/85 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> WIYN Open Cluster Study LXII: Comparison of Isochrone Systems using Deep Multi-Band Photometry of M35 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+B">Ben Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Frinchaboy%2C+P">Peter Frinchaboy</a>, <a href="/search/astro-ph?searchtype=author&query=Kinemuchi%2C+K">Karen Kinemuchi</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">Ata Sarajedini</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R">Roger Cohen</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="1408.1684v2-abstract-short" style="display: inline;"> Current generation stellar isochrone models exhibit non-negligible discrepancies due to variations in the input physics. The success of each model is determined by how well it fits the observations, and this paper aims to disentangle contributions from the various physical inputs. New deep, wide-field optical and near-infrared photometry ($UBVRIJHK_S$) of the cluster M35 is presented, against whic… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1408.1684v2-abstract-full').style.display = 'inline'; document.getElementById('1408.1684v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1408.1684v2-abstract-full" style="display: none;"> Current generation stellar isochrone models exhibit non-negligible discrepancies due to variations in the input physics. The success of each model is determined by how well it fits the observations, and this paper aims to disentangle contributions from the various physical inputs. New deep, wide-field optical and near-infrared photometry ($UBVRIJHK_S$) of the cluster M35 is presented, against which several isochrone systems are compared: Padova, PARSEC, Dartmouth and Y$^2$. Two different atmosphere models are applied to each isochrone: ATLAS9 and BT-Settl. For any isochrone set and atmosphere model, observed data are accurately reproduced for all stars more massive then $0.7$ M$_\odot$. For stars less massive than 0.7 M$_\odot$, Padova and PARSEC isochrones consistently produce higher temperatures than observed. Dartmouth and Y$^2$ isochrones with BT-Settl atmospheres reproduce optical data accurately, however they appear too blue in IR colors. It is speculated that molecular contributions to stellar spectra in the near-infrared may not be fully explored, and that future study may reconcile these differences. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1408.1684v2-abstract-full').style.display = 'none'; document.getElementById('1408.1684v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 August, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 August, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2014. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1407.0584">arXiv:1407.0584</a> <span> [<a href="https://arxiv.org/pdf/1407.0584">pdf</a>, <a href="https://arxiv.org/format/1407.0584">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/stu1327">10.1093/mnras/stu1327 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Void in the Sculptor Group Spiral Galaxy NGC 247 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wagner-Kaiser%2C+R">R. Wagner-Kaiser</a>, <a href="/search/astro-ph?searchtype=author&query=Demaio%2C+T">T. Demaio</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">A. Sarajedini</a>, <a href="/search/astro-ph?searchtype=author&query=Chakrabarti%2C+S">S. Chakrabarti</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="1407.0584v1-abstract-short" style="display: inline;"> The dwarf galaxy NGC 247, located in the Sculptor Filament, displays an apparent void on the north side of its spiral disk. The existence of the void in the disk of this dwarf galaxy has been known for some time, but the exact nature and cause of this strange feature has remained unclear. We investigate the properties of the void in the disk of NGC 247 using photometry of archival Hubble Space Tel… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1407.0584v1-abstract-full').style.display = 'inline'; document.getElementById('1407.0584v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1407.0584v1-abstract-full" style="display: none;"> The dwarf galaxy NGC 247, located in the Sculptor Filament, displays an apparent void on the north side of its spiral disk. The existence of the void in the disk of this dwarf galaxy has been known for some time, but the exact nature and cause of this strange feature has remained unclear. We investigate the properties of the void in the disk of NGC 247 using photometry of archival Hubble Space Telescope data to analyze the stars in and around this region. Based on a grid of isochrones from log(t)=6.8 to log(t)=10.0, we assign ages using nearest-neighbor interpolation. Examination of the spatial variation of these ages across the galaxy reveals an age difference between stars located inside the void region and stars located outside this region. We speculate that the void in NGC 247's stellar disk may be due to a recent interaction with a nearly dark sub-halo that collided with the disk and could account for the long-lived nature of the void. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1407.0584v1-abstract-full').style.display = 'none'; document.getElementById('1407.0584v1-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 July, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 10 figures, 3 tables. Accepted 2014 June 25. Received 2014 June 2; in original form 2014 March 25. MN-14-0765-MJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1404.1037">arXiv:1404.1037</a> <span> [<a href="https://arxiv.org/pdf/1404.1037">pdf</a>, <a href="https://arxiv.org/ps/1404.1037">ps</a>, <a href="https://arxiv.org/format/1404.1037">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/10.1088/0004-637X/786/2/147">10.1088/0004-637X/786/2/147 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The RR Lyrae Variable Population in the Phoenix Dwarf Galaxy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ordo%C3%B1ez%2C+A+J">Antonio J. Ordo帽ez</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+S">Soung-Chul Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">Ata Sarajedini</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="1404.1037v1-abstract-short" style="display: inline;"> We present the first detailed study of the RR Lyrae variable population in the Local Group dSph/dIrr transition galaxy, Phoenix, using previously obtained HST/WFPC2 observations of the galaxy. We utilize template light curve fitting routines to obtain best fit light curves for RR Lyrae variables in Phoenix. Our technique has identified 78 highly probable RR Lyrae stars (54 ab-type; 24 c-type) with… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1404.1037v1-abstract-full').style.display = 'inline'; document.getElementById('1404.1037v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1404.1037v1-abstract-full" style="display: none;"> We present the first detailed study of the RR Lyrae variable population in the Local Group dSph/dIrr transition galaxy, Phoenix, using previously obtained HST/WFPC2 observations of the galaxy. We utilize template light curve fitting routines to obtain best fit light curves for RR Lyrae variables in Phoenix. Our technique has identified 78 highly probable RR Lyrae stars (54 ab-type; 24 c-type) with about 40 additional candidates. We find mean periods for the two populations of $\langle P_{ab}\rangle = 0.60 \pm 0.03$ days and $\langle P_{c}\rangle = 0.353 \pm 0.002$ days. We use the properties of these light curves to extract, among other things, a metallicity distribution function for ab-type RR Lyrae. Our analysis yields a mean metallicity of $\langle [Fe/H]\rangle = -1.68 \pm 0.06$ dex for the RRab stars. From the mean period and metallicity calculated from the ab-type RR Lyrae, we conclude that Phoenix is more likely of intermediate Oosterhoff type; however the morphology of the Bailey diagram for Phoenix RR Lyraes appears similar to that of an Oosterhoff type I system. Using the RRab stars, we also study the chemical enrichment law for Phoenix. We find that our metallicity distribution is reasonably well fitted by a closed-box model. The parameters of this model are compatible with the findings of Hidalgo et al. (2009) further supporting the idea that Phoenix appears to have been chemically enriched as a closed-box-like system during the early stage of its formation and evolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1404.1037v1-abstract-full').style.display = 'none'; document.getElementById('1404.1037v1-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 April, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 16 figures, 6 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Ordo帽ez, A. J., Yang, S.-C., and Sarajedini, A, 2014, ApJ, 786, 147 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1402.3874">arXiv:1402.3874</a> <span> [<a href="https://arxiv.org/pdf/1402.3874">pdf</a>, <a href="https://arxiv.org/ps/1402.3874">ps</a>, <a href="https://arxiv.org/format/1402.3874">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/784/1/76">10.1088/0004-637X/784/1/76 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Early Chemical Enrichment Histories of Two Sculptor Group Dwarf Galaxies as Revealed by RR Lyrae Variables </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Yang%2C+S">Soung-Chul Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Wagner-Kaiser%2C+R">Rachel Wagner-Kaiser</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">Ata Sarajedini</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S+C">Sang Chul Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kyeong%2C+J">Jaemann Kyeong</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="1402.3874v1-abstract-short" style="display: inline;"> We present the results of our analysis of the RR Lyrae (RRL) variable stars detected in two transition-type dwarf galaxies (dTrans), ESO294-G010 and ESO410-G005 in the Sculptor group, which is known to be one of the closest neighboring galaxy groups to our Local Group. Using deep archival images from the Advanced Camera for Surveys (ACS) onboard the Hubble Space Telescope (HST), we have identified… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1402.3874v1-abstract-full').style.display = 'inline'; document.getElementById('1402.3874v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1402.3874v1-abstract-full" style="display: none;"> We present the results of our analysis of the RR Lyrae (RRL) variable stars detected in two transition-type dwarf galaxies (dTrans), ESO294-G010 and ESO410-G005 in the Sculptor group, which is known to be one of the closest neighboring galaxy groups to our Local Group. Using deep archival images from the Advanced Camera for Surveys (ACS) onboard the Hubble Space Telescope (HST), we have identified a sample of RR Lyrae candidates in both dTrans galaxies [219 RRab (RR0) and 13 RRc (RR1) variables in ESO294-G010; 225 RRab and 44 RRc stars in ESO410-G005]. The metallicities of the individual RRab stars are calculated via the period-amplitude-[Fe/H] relation derived by Alcock et al. This yields mean metallicities of <[Fe/H]>_{ESO294} = -1.77 +/- 0.03 and <[Fe/H]>_{ESO410} = -1.64 +/- 0.03. The RRL metallicity distribution functions (MDFs) are investigated further via simple chemical evolution models; these reveal the relics of the early chemical enrichment processes for these two dTrans galaxies. In the case of both galaxies, the shapes of the RRL MDFs are well-described by pre-enrichment models. This suggests two possible channels for the early chemical evolution for these Sculptor group dTrans galaxies: 1) The ancient stellar populations of our target dwarf galaxies might have formed from the star forming gas which was already enriched through "prompt initial enrichment" or an "initial nucleosynthetic spike" from the very first massive stars, or 2) this pre-enrichment state might have been achieved by the end products from more evolved systems of their nearest neighbor, NGC 55. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1402.3874v1-abstract-full').style.display = 'none'; document.getElementById('1402.3874v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 February, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 17 figures, accepted to 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/1402.1687">arXiv:1402.1687</a> <span> [<a href="https://arxiv.org/pdf/1402.1687">pdf</a>, <a href="https://arxiv.org/ps/1402.1687">ps</a>, <a href="https://arxiv.org/format/1402.1687">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/10.1088/0004-6256/147/4/71">10.1088/0004-6256/147/4/71 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Age Determination of Fifteen Old to Intermediate-Age Small Magellanic Cloud Star Clusters </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=Geisler%2C+D">D. Geisler</a>, <a href="/search/astro-ph?searchtype=author&query=Carraro%2C+G">G. Carraro</a>, <a href="/search/astro-ph?searchtype=author&query=Clari%C3%A1%2C+J+J">J. J. Clari谩</a>, <a href="/search/astro-ph?searchtype=author&query=Costa%2C+E">E. Costa</a>, <a href="/search/astro-ph?searchtype=author&query=Grocholski%2C+A+J">A. J. Grocholski</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">A. Sarajedini</a>, <a href="/search/astro-ph?searchtype=author&query=Leiton%2C+R">R. Leiton</a>, <a href="/search/astro-ph?searchtype=author&query=Piatti%2C+A+E">A. E. Piatti</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="1402.1687v1-abstract-short" style="display: inline;"> We present CMDs in the V and I bands for fifteen star clusters in the Small Magellanic Cloud (SMC) based on data taken with the Very Large Telescope (VLT, Chile). We selected these clusters from our previous work, wherein we derived cluster radial velocities and metallicities from Calcium II infrared triplet (CaT) spectra also taken with the VLT. We discovered that the ages of six of our clusters… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1402.1687v1-abstract-full').style.display = 'inline'; document.getElementById('1402.1687v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1402.1687v1-abstract-full" style="display: none;"> We present CMDs in the V and I bands for fifteen star clusters in the Small Magellanic Cloud (SMC) based on data taken with the Very Large Telescope (VLT, Chile). We selected these clusters from our previous work, wherein we derived cluster radial velocities and metallicities from Calcium II infrared triplet (CaT) spectra also taken with the VLT. We discovered that the ages of six of our clusters have been appreciably underestimated by previous studies, which used comparatively small telescopes, graphically illustrating the need for large apertures to obtain reliable ages of old and intermediate-age SMC star clusters. In particular, three of these clusters, L4, L6 and L110, turn out to be amongst the oldest SMC clusters known, with ages of 7.9 +- 1.1, 8.7 +- 1.2 and 7.6 +- 1.0 Gyr, respectively, helping to fill a possible "SMC cluster age gap" (Glatt et al. 2008). Using the present ages and metallicities from Parisi et al. (2009), we analyze the age distribution, age gradient and age metallicity relation (AMR) of a sample of SMC clusters measured homogeneously. There is a suggestion of bimodality in the age distribution but it does not show a constant slope for the first 4 Gyr (Piatti 2011), and we find no evidence for an age gradient. Due to the improved ages of our cluster sample, we find that our AMR is now better represented in the intermediate/old period than that we derived in Parisi et al. (2009), where we simply took ages available in the literature. Additionally, clusters younger than aprox. 4 Gyr now show better agreement with the bursting model, but we confirm that this model is not a good representation of the AMR during the intermediate-age/old period. A more complicated model is needed to explain the SMC chemical evolution in that period. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1402.1687v1-abstract-full').style.display = 'none'; document.getElementById('1402.1687v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 February, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">76 pages, 32 figures. Accepted for publication in AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1312.4169">arXiv:1312.4169</a> <span> [<a href="https://arxiv.org/pdf/1312.4169">pdf</a>, <a href="https://arxiv.org/ps/1312.4169">ps</a>, <a href="https://arxiv.org/format/1312.4169">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/10.1088/0004-637X/785/1/21">10.1088/0004-637X/785/1/21 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Global and non-global parameters of horizontal branch morphology of globular clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Milone%2C+A+P">A. P. Milone</a>, <a href="/search/astro-ph?searchtype=author&query=Marino%2C+A+F">A. F. Marino</a>, <a href="/search/astro-ph?searchtype=author&query=Dotter%2C+A">A. Dotter</a>, <a href="/search/astro-ph?searchtype=author&query=Norris%2C+J+E">J. E. Norris</a>, <a href="/search/astro-ph?searchtype=author&query=Jerjen%2C+H">H. Jerjen</a>, <a href="/search/astro-ph?searchtype=author&query=Piotto%2C+G">G. Piotto</a>, <a href="/search/astro-ph?searchtype=author&query=Cassisi%2C+S">S. Cassisi</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=Blanco%2C+A+R">A. Recio Blanco</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">A. Sarajedini</a>, <a href="/search/astro-ph?searchtype=author&query=Asplund%2C+M">M. Asplund</a>, <a href="/search/astro-ph?searchtype=author&query=Monelli%2C+M">M. Monelli</a>, <a href="/search/astro-ph?searchtype=author&query=Aparicio%2C+A">A. Aparicio</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="1312.4169v1-abstract-short" style="display: inline;"> The horizontal branch (HB) morphology of globular clusters (GCs) is mainly determined by metallicity. However, the fact that GCs with almost the same metallicity exhibit different HB morphologies demonstrates that at least one more parameter is needed to explain the HB morphology. It has been suggested that one of these should be a global parameter that varies from GC to GC, and the other a non-gl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1312.4169v1-abstract-full').style.display = 'inline'; document.getElementById('1312.4169v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1312.4169v1-abstract-full" style="display: none;"> The horizontal branch (HB) morphology of globular clusters (GCs) is mainly determined by metallicity. However, the fact that GCs with almost the same metallicity exhibit different HB morphologies demonstrates that at least one more parameter is needed to explain the HB morphology. It has been suggested that one of these should be a global parameter that varies from GC to GC, and the other a non-global parameter that varies within the GC. In this study we provide empirical evidence corroborating this idea. We used the photometric catalogs obtained with the Advanced Camera for Surveys (ACS) of the Hubble Space Telescope (HST) and analyse the CMDs of 74 GCs. The HB morphology of our sample of GCs has been investigated on the basis of the two new parameters L1 and L2 that measure the distance between the RGB and the coolest part of the HB, and the color extension of the HB, respectively. We find that L1 correlates with both metallicity and age, whereas L2 most strongly correlates with the mass of the hosting GC. The range of helium abundance among the stars in a GC, characterised by Delta Y and associated with the presence of multiple stellar populations, has been estimated in a few GCs to date. In these GCs we find a close relationship among Delta Y, GC mass, and L2. We conclude that age and metallicity are the main global parameters while the range of helium abundance within a GC is the main non-global parameter defining the HB morphology of Galactic GCs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1312.4169v1-abstract-full').style.display = 'none'; document.getElementById('1312.4169v1-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, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2013. </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">34 pages, 13 figures, accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1312.1641">arXiv:1312.1641</a> <span> [<a href="https://arxiv.org/pdf/1312.1641">pdf</a>, <a href="https://arxiv.org/ps/1312.1641">ps</a>, <a href="https://arxiv.org/format/1312.1641">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0067-0049/211/1/1">10.1088/0067-0049/211/1/1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The ACS survey of globular clusters. XIII. Photometric calibration in comparison with Stetson standards </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hempel%2C+M">Maren Hempel</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">Ata Sarajedini</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">Jay Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Aparicio%2C+A">Antonio Aparicio</a>, <a href="/search/astro-ph?searchtype=author&query=Bedin%2C+L+R">Luigi R. Bedin</a>, <a href="/search/astro-ph?searchtype=author&query=Chaboyer%2C+B">Brian Chaboyer</a>, <a href="/search/astro-ph?searchtype=author&query=Majewski%2C+S+R">Steven R. Majewski</a>, <a href="/search/astro-ph?searchtype=author&query=Mar%C3%ADn-Franch%2C+A">Antonio Mar铆n-Franch</a>, <a href="/search/astro-ph?searchtype=author&query=Milone%2C+A">Antonino Milone</a>, <a href="/search/astro-ph?searchtype=author&query=Paust%2C+N+E+Q">Nathaniel E. Q. Paust</a>, <a href="/search/astro-ph?searchtype=author&query=Piotto%2C+G">Giampaolo Piotto</a>, <a href="/search/astro-ph?searchtype=author&query=Reid%2C+I+N">I. Neill Reid</a>, <a href="/search/astro-ph?searchtype=author&query=Rosenberg%2C+A">Alfred Rosenberg</a>, <a href="/search/astro-ph?searchtype=author&query=Siegel%2C+M">Michael Siegel</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="1312.1641v1-abstract-short" style="display: inline;"> In this study we compare the photometric data of 34 Milky Way globular clusters, observed within the ACS Treasury Program (PI: Ata Sarajedini) with the corresponding ground-based data, provided by the Photometric Standard Field Catalogs of Stetson (2000, 2005). We focus on the transformation between the HST/ACS F606W to V-band and F814W to I-band only. The goal is to assess the validity of the fil… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1312.1641v1-abstract-full').style.display = 'inline'; document.getElementById('1312.1641v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1312.1641v1-abstract-full" style="display: none;"> In this study we compare the photometric data of 34 Milky Way globular clusters, observed within the ACS Treasury Program (PI: Ata Sarajedini) with the corresponding ground-based data, provided by the Photometric Standard Field Catalogs of Stetson (2000, 2005). We focus on the transformation between the HST/ACS F606W to V-band and F814W to I-band only. The goal is to assess the validity of the filter transformation equations by Sirianni et al.(2005) with respect to their dependence on metallicity, Horizontal Branch morphology, mass and integrated (V-I) colour of the various globular clusters. Such a dependence is expected due to the fact that the transformation equations are based on the observations of only one globular cluster, i.e., NGC 2419. Surprisingly, the correlation between offset and metallicity is found to be weak, with a low level significance. The correlation between offset and Horizontal Branch structure, as well as total cluster mass is still weaker. Based on the available data we do not find the photometric offset to be linked to multiple stellar populations, e.g., as found in NGC 0288, NGC 1851, and NGC 5139. The results of this study show that there are small systematic offsets between the transformed ACS- and observed ground based photometry, and that these are only weakly correlated, if at all, with various cluster parameters and their underlying stellar populations. As a result, investigators wishing to transform globular cluster photometry from the Sirianni et al.(2005) ground-based V, I system onto the Stetson (2000) system simply need to add 0.040 (+/-0.012) to the V-band magnitudes and 0.047 (+/-0.011) to the I-band magnitudes. This in turn means that the transformed ACS (V-I) colours match the ground-based values from Stetson (2000) to within ~0.01 mag. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1312.1641v1-abstract-full').style.display = 'none'; document.getElementById('1312.1641v1-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 December, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages, 14 figures, accepted for publication in ApJS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1308.6252">arXiv:1308.6252</a> <span> [<a href="https://arxiv.org/pdf/1308.6252">pdf</a>, <a href="https://arxiv.org/ps/1308.6252">ps</a>, <a href="https://arxiv.org/format/1308.6252">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-6256/146/5/109">10.1088/0004-6256/146/5/109 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Three New Galactic Center X-ray Sources Identified with Near-Infrared Spectroscopy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=DeWitt%2C+C">Curtis DeWitt</a>, <a href="/search/astro-ph?searchtype=author&query=Bandyopadhyay%2C+R+M">Reba M. Bandyopadhyay</a>, <a href="/search/astro-ph?searchtype=author&query=Eikenberry%2C+S+S">Stephen S. Eikenberry</a>, <a href="/search/astro-ph?searchtype=author&query=Sellgren%2C+K">Kris Sellgren</a>, <a href="/search/astro-ph?searchtype=author&query=Blum%2C+R">Robert Blum</a>, <a href="/search/astro-ph?searchtype=author&query=Olsen%2C+K">Knut Olsen</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">Ata Sarajedini</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="1308.6252v1-abstract-short" style="display: inline;"> We have conducted a near-infrared spectroscopic survey of 47 candidate counterparts to X-ray sources discovered by the Chandra X-ray Observatory near the Galactic Center (GC). Though a significant number of these astrometric matches are likely to be spurious, we sought out spectral characteristics of active stars and interacting binaries, such as hot, massive spectral types or emission lines in or… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1308.6252v1-abstract-full').style.display = 'inline'; document.getElementById('1308.6252v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1308.6252v1-abstract-full" style="display: none;"> We have conducted a near-infrared spectroscopic survey of 47 candidate counterparts to X-ray sources discovered by the Chandra X-ray Observatory near the Galactic Center (GC). Though a significant number of these astrometric matches are likely to be spurious, we sought out spectral characteristics of active stars and interacting binaries, such as hot, massive spectral types or emission lines in order to corroborate the X-ray activity and certify the authenticity of the match. We present three new spectroscopic identifications, including a Be high mass X-ray binary (HMXB) or a gamma Cassiopeiae (Cas) system, a symbiotic X-ray binary and an O-type star of unknown luminosity class. The Be HMXB/gamma Cas system and the symbiotic X-ray binary are the first of their classes to be spectroscopically identified in the GC region. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1308.6252v1-abstract-full').style.display = 'none'; document.getElementById('1308.6252v1-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 August, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">33 pages, 12 figures, AJ accepted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1302.2827">arXiv:1302.2827</a> <span> [<a href="https://arxiv.org/pdf/1302.2827">pdf</a>, <a href="https://arxiv.org/ps/1302.2827">ps</a>, <a href="https://arxiv.org/format/1302.2827">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/stt277">10.1093/mnras/stt277 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Properties of the Large Magellanic Cloud Based on OGLE III Photometry of RR Lyrae Stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wagner-Kaiser%2C+R">Rachel Wagner-Kaiser</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">Ata Sarajedini</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="1302.2827v1-abstract-short" style="display: inline;"> We present results from a study of ab-type RR Lyrae variables in the Large Magellanic Cloud using the extensive dataset from phase III of the Optical Gravitational Lensing Experiment (OGLE). The metallicities of the RR Lyraes, determined from the periods and amplitudes of their light curves, reveal a statistically significant radial abundance gradient that is approximately one-half of what is seen… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1302.2827v1-abstract-full').style.display = 'inline'; document.getElementById('1302.2827v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1302.2827v1-abstract-full" style="display: none;"> We present results from a study of ab-type RR Lyrae variables in the Large Magellanic Cloud using the extensive dataset from phase III of the Optical Gravitational Lensing Experiment (OGLE). The metallicities of the RR Lyraes, determined from the periods and amplitudes of their light curves, reveal a statistically significant radial abundance gradient that is approximately one-half of what is seen in the disks of the Milky Way and M33. The RR Lyrae abundance gradient agrees with that of the old and metal-poor LMC globular clusters. The reddenings of the OGLE RR Lyraes have been calculated using their minimum light colors and reveal a mean value of E(V-I) = 0.12 +/- 0.05, where the quoted uncertainty represents the standard deviation of the mean. The distribution of RR Lyrae extinctions across the face of the LMC is well-correlated with the distribution and emission intensity of CO clouds based on recent millimeter wave surveys. In addition, we find that the old LMC globulars tend to be located in regions of low extinction. This underscores the need to survey the higher extinction regions with the specific aim of increasing the sample of old LMC globular clusters. Finally, we examine the distance distribution of the RR Lyraes in order to probe the structure of the LMC and investigate the possibility that some of the RR Lyraes may reside in a kinematically hot halo population. In addition to calculating a mean LMC distance of (m-M)o = 18.55 +/- 0.10 mag, we conclude that some fraction of the RR Lyraes in our sample could be members of the LMC halo. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1302.2827v1-abstract-full').style.display = 'none'; document.getElementById('1302.2827v1-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 February, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2013. </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">ref. MN-12-2095-MJ.R2 Accepted 2013 February 11. Received 2013 February 10; in original form 2012 August 25</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1301.2822">arXiv:1301.2822</a> <span> [<a href="https://arxiv.org/pdf/1301.2822">pdf</a>, <a href="https://arxiv.org/ps/1301.2822">ps</a>, <a href="https://arxiv.org/format/1301.2822">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/10.1088/0004-637X/765/1/32">10.1088/0004-637X/765/1/32 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The intriguing stellar populations in the globular clusters NGC 6388 and NGC 6441 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">A. Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Piotto%2C+G">G. Piotto</a>, <a href="/search/astro-ph?searchtype=author&query=Milone%2C+A+P">A. P. Milone</a>, <a href="/search/astro-ph?searchtype=author&query=King%2C+I+R">I. R. King</a>, <a href="/search/astro-ph?searchtype=author&query=Renzini%2C+A">A. Renzini</a>, <a href="/search/astro-ph?searchtype=author&query=Cassisi%2C+S">S. Cassisi</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">J. Anderson</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=Nardiello%2C+D">D. Nardiello</a>, <a href="/search/astro-ph?searchtype=author&query=Pietrinferni%2C+A">A. Pietrinferni</a>, <a href="/search/astro-ph?searchtype=author&query=Sarajedini%2C+A">A. Sarajedini</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="1301.2822v1-abstract-short" style="display: inline;"> NGC 6388 and NGC 6441 are two massive Galactic bulge globular clusters which share many properties, including the presence of an extended horizontal branch (HB), quite unexpected because of their high metal content. In this paper we use HST's WFPC2, ACS, and WFC3 images and present a broad multicolor study of their stellar content, covering all main evolutionary branches. The color-magnitude diagr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1301.2822v1-abstract-full').style.display = 'inline'; document.getElementById('1301.2822v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1301.2822v1-abstract-full" style="display: none;"> NGC 6388 and NGC 6441 are two massive Galactic bulge globular clusters which share many properties, including the presence of an extended horizontal branch (HB), quite unexpected because of their high metal content. In this paper we use HST's WFPC2, ACS, and WFC3 images and present a broad multicolor study of their stellar content, covering all main evolutionary branches. The color-magnitude diagrams (CMDs) give compelling evidence that both clusters host at least two stellar populations, which manifest themselves in different ways. NGC 6388 has a broadened main sequence (MS), a split sub-giant branch (SGB), and a split red giant branch (RGB) that becomes evident above the HB in our data set; its red HB is also split into two branches. NGC 6441 has a split MS, but only an indication of two SGB populations, while the RGB clearly splits in two from the SGB level upward, and no red HB structure. The multicolor analysis of the CMDs confirms that the He difference between the two main stellar populations in the two clusters must be similar. This is observationally supported by the HB morphology, but also confirmed by the color distribution of the stars in the MS optical band CMDs. However, a MS split becomes evident in NGC 6441 using UV colors, but not in NGC 6388, indicating that the chemical patterns of the different populations are different in the two clusters, with C, N, O abundance differences likely playing a major role. We also analyze the radial distribution of the two populations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1301.2822v1-abstract-full').style.display = 'none'; document.getElementById('1301.2822v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 January, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2013. </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">31 pages, 26 figures (some in low res to fit within astroph 15 MB limit), 7 tables, accepted for publication in the Astrophysical Journal</span> </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous 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