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</div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.05376">arXiv:2412.05376</a> <span> [<a href="https://arxiv.org/pdf/2412.05376">pdf</a>, <a href="https://arxiv.org/format/2412.05376">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Binary and Grouped Open Clusters: A New Catalogue </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Palma%2C+T">Tali Palma</a>, <a href="/search/astro-ph?searchtype=author&query=Coenda%2C+V">Valeria Coenda</a>, <a href="/search/astro-ph?searchtype=author&query=Baume%2C+G">Gustavo Baume</a>, <a href="/search/astro-ph?searchtype=author&query=Feinstein%2C+C">Carlos Feinstein</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2412.05376v1-abstract-short" style="display: inline;"> Context. Understanding the formation and evolution of star clusters in the Milky Way requires precise identification of clusters that form binary or multiple systems. Such systems offer valuable insight into the dynamical processes and interactions that influence cluster evolution. Aims. This study aims to identify and classify star clusters in the Milky Way as part of double or multiple systems.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.05376v1-abstract-full').style.display = 'inline'; document.getElementById('2412.05376v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.05376v1-abstract-full" style="display: none;"> Context. Understanding the formation and evolution of star clusters in the Milky Way requires precise identification of clusters that form binary or multiple systems. Such systems offer valuable insight into the dynamical processes and interactions that influence cluster evolution. Aims. This study aims to identify and classify star clusters in the Milky Way as part of double or multiple systems. Specifically, we seek to detect clusters that form gravitationally bound pairs or groups of clusters and distinguish between different types of interactions based on their physical properties and spatial distributions. Methods. We used the extensive star cluster database of Hunt & Reffert (2023, 2024), which includes 7167 clusters. By estimating the tidal forces acting on each cluster through the tidal factor (TF), and considering only close neighbours (within 50 pc), we identified a total of 2170 star clusters forming part of double and multiple systems. Pairs were classified as Binaries (B), Capture pairs (C), or Optical pairs (O/Oa) based on proper motion distributions, cluster ages, and color-magnitude diagrams. Results. Our analysis identified 617 paired systems, which were successfully classified using our scheme. Additionally, we found 261 groups of star clusters, each with three or more members, further supporting the presence of multiple systems within the Milky Way that exhibit significant tidal interactions. Conclusions. The method presented provides an improved approach for identifying star clusters that share the same spatial volume and experience notable tidal interactions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.05376v1-abstract-full').style.display = 'none'; document.getElementById('2412.05376v1-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 11 figures, 3 tables. Accepted for Publication in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.09756">arXiv:2312.09756</a> <span> [<a href="https://arxiv.org/pdf/2312.09756">pdf</a>, <a href="https://arxiv.org/format/2312.09756">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> The VISCACHA survey -- IX. The SMC Southern Bridge in 8D </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Parisi%2C+M+C">M. C. Parisi</a>, <a href="/search/astro-ph?searchtype=author&query=Oliveira%2C+R+A+P">R. A. P. Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Angelo%2C+M">M. Angelo</a>, <a href="/search/astro-ph?searchtype=author&query=Dias%2C+B">B. Dias</a>, <a href="/search/astro-ph?searchtype=author&query=Maia%2C+F">F. Maia</a>, <a href="/search/astro-ph?searchtype=author&query=Saroon%2C+S">S. Saroon</a>, <a href="/search/astro-ph?searchtype=author&query=Feinstein%2C+C">C. Feinstein</a>, <a href="/search/astro-ph?searchtype=author&query=Santos%2C+J+F+C">J. F. C. Santos Jr.</a>, <a href="/search/astro-ph?searchtype=author&query=Bica%2C+E">E. Bica</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+B+P+L">B. Pereira Lima Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez-Trincado%2C+J+G">J. G. Fern谩ndez-Trincado</a>, <a href="/search/astro-ph?searchtype=author&query=Westera%2C+P">P. Westera</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Garro%2C+E+R">E. R. Garro</a>, <a href="/search/astro-ph?searchtype=author&query=Santrich%2C+O+J+K">O. J. Katime Santrich</a>, <a href="/search/astro-ph?searchtype=author&query=De+Bortoli%2C+B">B. De Bortoli</a>, <a href="/search/astro-ph?searchtype=author&query=Souza%2C+S">S. Souza</a>, <a href="/search/astro-ph?searchtype=author&query=Kerber%2C+L">L. Kerber</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A9rez-Villegas%2C+A">A. P茅rez-Villegas</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.09756v1-abstract-short" style="display: inline;"> The structure of the Small Magellanic Cloud (SMC) outside of its main body is characterised by tidal branches resulting from its interactions mainly with the Large Magellanic Cloud (LMC). Characterising the stellar populations in these tidal components helps to understand the dynamical history of this galaxy and of the Magellanic system in general. We provide full phase-space vector information fo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.09756v1-abstract-full').style.display = 'inline'; document.getElementById('2312.09756v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.09756v1-abstract-full" style="display: none;"> The structure of the Small Magellanic Cloud (SMC) outside of its main body is characterised by tidal branches resulting from its interactions mainly with the Large Magellanic Cloud (LMC). Characterising the stellar populations in these tidal components helps to understand the dynamical history of this galaxy and of the Magellanic system in general. We provide full phase-space vector information for Southern Bridge clusters. We performed a photometric and spectroscopic analysis of twelve SMC clusters, doubling the number of SMC clusters with full phase-space vector information known to date. We reclassify the sample considering 3D distances and 3D velocities. We found that some of the clusters classified as Southern Bridge objects according to the projected 2D classification actually belong to the Main Body and Counter-Bridge in the background. The comparison of the kinematics of the genuine foreground Bridge clusters with those previously analysed in the same way reveals that Southern Bridge clusters are moving towards the LMC and share the kinematics of the Northern Bridge. Adding to our sample clusters from the literature with CaT metallicity determinations we compare the age-metallicity relation of the Southern Bridge with the one of the Northern Bridge. We reinforce the idea that both regions do not seem to have experienced the same chemical enrichment history and that there is a clear absence of clusters in the Northern Bridge older than 3Gyr and more metal-poor than -1.1, which would not seem to be due to a selection effect. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.09756v1-abstract-full').style.display = 'none'; document.getElementById('2312.09756v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 9 figures, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.09685">arXiv:2212.09685</a> <span> [<a href="https://arxiv.org/pdf/2212.09685">pdf</a>, <a href="https://arxiv.org/format/2212.09685">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> The VISCACHA survey -- VI. Dimensional study of the structure of 82 star clusters in the Magellanic Clouds </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rodr%C3%ADguez%2C+M+J">M. Jimena Rodr铆guez</a>, <a href="/search/astro-ph?searchtype=author&query=Feinstein%2C+C">C. Feinstein</a>, <a href="/search/astro-ph?searchtype=author&query=Baume%2C+G">G. Baume</a>, <a href="/search/astro-ph?searchtype=author&query=Dias%2C+B">B. Dias</a>, <a href="/search/astro-ph?searchtype=author&query=Maia%2C+F+S+M">F. S. M. Maia</a>, <a href="/search/astro-ph?searchtype=author&query=Santos%2C+J+F+C">J. F. C. Santos Jr.</a>, <a href="/search/astro-ph?searchtype=author&query=Kerber%2C+L">L. Kerber</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A9rez-Villegas%2C+A">A. P茅rez-Villegas</a>, <a href="/search/astro-ph?searchtype=author&query=De+B%C3%B3rtoli%2C+B">B. De B贸rtoli</a>, <a href="/search/astro-ph?searchtype=author&query=Parisi%2C+M+C">M. C. Parisi</a>, <a href="/search/astro-ph?searchtype=author&query=Oliveira%2C+R+A+P">R. A. P. Oliveira</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2212.09685v1-abstract-short" style="display: inline;"> We present a study of the internal structure of 82 star clusters located at the outer regions of the Large Magellanic Cloud and the Small Magellanic Cloud using data of the VISCACHA Survey. Through the construction of the minimum spanning tree, which analyzes the relative position of stars within a given cluster, it was possible to characterize the internal structure and explore the fractal or sub… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.09685v1-abstract-full').style.display = 'inline'; document.getElementById('2212.09685v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.09685v1-abstract-full" style="display: none;"> We present a study of the internal structure of 82 star clusters located at the outer regions of the Large Magellanic Cloud and the Small Magellanic Cloud using data of the VISCACHA Survey. Through the construction of the minimum spanning tree, which analyzes the relative position of stars within a given cluster, it was possible to characterize the internal structure and explore the fractal or subclustered distribution for each cluster. We computed the parameters m (which is the average length of the connected segments normalized by the area), s (which is the mean points separation in units of cluster radius), and Q (the ratio of these components). These parameters are useful to distinguish between radial, homogeneous, and substructured distributions of stars. The dependence of these parameters with the different characteristics of the clusters, such as their ages and spatial distribution, was also studied. We found that most of the studied clusters present a homogeneous stellar distribution or a distribution with a radial concentration. Our results are consistent with the models, suggesting that more dynamically evolved clusters seem to have larger Q values, confirming previous results from numerical simulations. There also seems to be a correlation between the internal structure of the clusters and their galactocentric distances, in the sense that for both galaxies, the more distant clusters have larger Q values. We also paid particular attention to the effects of contamination by non-member field stars and its consequences finding that field star decontamination is crucial for these kinds of studies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.09685v1-abstract-full').style.display = 'none'; document.getElementById('2212.09685v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 11 figures, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2010.14419">arXiv:2010.14419</a> <span> [<a href="https://arxiv.org/pdf/2010.14419">pdf</a>, <a href="https://arxiv.org/format/2010.14419">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202038970">10.1051/0004-6361/202038970 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Hierarchical star formation in nearby galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rodr%C3%ADguez%2C+M+J">Mar铆a Jimena Rodr铆guez</a>, <a href="/search/astro-ph?searchtype=author&query=Baume%2C+G">Gustavo Baume</a>, <a href="/search/astro-ph?searchtype=author&query=Feinstein%2C+C">Carlos Feinstein</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2010.14419v1-abstract-short" style="display: inline;"> Aims: The purpose of this work is to study the properties of the spatial distribution of the young population in three nearby galaxies in order to better understand the first stages of star formation. Methods: We used ACS/HST photometry and the "path-linkage criterion" in order to obtain a catalog of young stellar groups (YSGs) in the galaxy NGC 2403. We studied the internal distribution of star… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.14419v1-abstract-full').style.display = 'inline'; document.getElementById('2010.14419v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.14419v1-abstract-full" style="display: none;"> Aims: The purpose of this work is to study the properties of the spatial distribution of the young population in three nearby galaxies in order to better understand the first stages of star formation. Methods: We used ACS/HST photometry and the "path-linkage criterion" in order to obtain a catalog of young stellar groups (YSGs) in the galaxy NGC 2403. We studied the internal distribution of stars in these YSGs using the Q parameter. We extended these analyses to the YSGs detected in in NGC 300 and NGC 253 our previous works. We built the young stars' density maps for these three galaxies. Through these maps, we were able to identify and study young stellar structures on larger scales. Results: We found 573 YSGs in the galaxy NGC 2403, for which we derived their individual sizes, densities, luminosity function,and other fundamental characteristics. We find that the vast majority of the YSGs in NGC 2403, NGC 300 and NGC 253 present inner clumpings, following the same hierarchical behavior that we observed in the young stellar structures on larger scales in these galaxies. We derived values of the fractal dimension for these structures between ~ 1.5 and 1.6. These values are very similar to those obtained in other star forming galaxies and in the interstellar medium, suggesting that the star formation process is regulated by supersonic turbulence. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.14419v1-abstract-full').style.display = 'none'; document.getElementById('2010.14419v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 10 figures, 2 tables, Accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 644, A101 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1904.09926">arXiv:1904.09926</a> <span> [<a href="https://arxiv.org/pdf/1904.09926">pdf</a>, <a href="https://arxiv.org/format/1904.09926">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201935291">10.1051/0004-6361/201935291 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The young stellar population in NGC 247 Main properties and hierarchical clustering </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rodr%C3%ADguez%2C+M+J">M. J. Rodr铆guez</a>, <a href="/search/astro-ph?searchtype=author&query=Baume%2C+G">G. Baume</a>, <a href="/search/astro-ph?searchtype=author&query=Feinstein%2C+C">C. Feinstein</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="1904.09926v1-abstract-short" style="display: inline;"> The aim of this work is to investigate the characteristics of the young stellar population in the spiral galaxy NGC 247. In particular, we focused our attention in its hierarchical clustering distributions and the properties of the smallest groups. We used multiband Hubble Space Telescope (HST) data from three fields covering more than half of NGC 247 to select the young population. Then, through… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.09926v1-abstract-full').style.display = 'inline'; document.getElementById('1904.09926v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1904.09926v1-abstract-full" style="display: none;"> The aim of this work is to investigate the characteristics of the young stellar population in the spiral galaxy NGC 247. In particular, we focused our attention in its hierarchical clustering distributions and the properties of the smallest groups. We used multiband Hubble Space Telescope (HST) data from three fields covering more than half of NGC 247 to select the young population. Then, through the path linkage criterion (PLC), we found compact young star groups, and estimated their fundamental parameters, such as their stellar densities, sizes, amount of members and luminosity function (LF) slopes. We also performed a fractal analysis to determinate the clustering properties of this population. We build a stellar density map and the corresponding dendrograms corresponding to the galactic young population to detect large structures and draw their main characteristics. We detected 339 young star groups, for which we computed a mean radius of $\sim$ 60 pc and a maximum in the size distribution between 30 and 70 pc. We also obtained LF slopes with a bimodal distribution showing peaks at $\sim$ 0.1 and $\sim$ 0.2. We identified several candidates to HII regions which follow an excellent spatial correlation with the young groups found by the PLC. We observed that the young population are hierarchically organized, where the smaller and denser structures are within larger and less dense ones. We noticed that all these groups presented a fractal subclustering, following the hierarchical distribution observed in the corresponding stellar density map. For the large young structures observed in this map, we obtained a fractal dimension of $\sim$ 1.6-1.8 using the perimeter-area relation and the cumulative size distribution. These values are consistent with a scenario of hierarchical star formation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.09926v1-abstract-full').style.display = 'none'; document.getElementById('1904.09926v1-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 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">Accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 626, A35 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1903.10989">arXiv:1903.10989</a> <span> [<a href="https://arxiv.org/pdf/1903.10989">pdf</a>, <a href="https://arxiv.org/ps/1903.10989">ps</a>, <a href="https://arxiv.org/format/1903.10989">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 stellar photometry and the blending problem </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Feinstein%2C+C">C. Feinstein</a>, <a href="/search/astro-ph?searchtype=author&query=Baume%2C+G">G. Baume</a>, <a href="/search/astro-ph?searchtype=author&query=Rodriguez%2C+J">J. Rodriguez</a>, <a href="/search/astro-ph?searchtype=author&query=Vergne%2C+M">M. Vergne</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="1903.10989v1-abstract-short" style="display: inline;"> The images provided by the Advanced Camera for Surveys at the Hubble Space Telescope (ACS/HST) have the amazing spacial resolution of 0".05/pixel. Therefore, it is possible to resolve individual stars in nearby galaxies and, in particular, young blue stars in associations and open clusters of the recent starburst. These data are useful for studies of the extragalactic young population using color… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.10989v1-abstract-full').style.display = 'inline'; document.getElementById('1903.10989v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1903.10989v1-abstract-full" style="display: none;"> The images provided by the Advanced Camera for Surveys at the Hubble Space Telescope (ACS/HST) have the amazing spacial resolution of 0".05/pixel. Therefore, it is possible to resolve individual stars in nearby galaxies and, in particular, young blue stars in associations and open clusters of the recent starburst. These data are useful for studies of the extragalactic young population using color magnitude diagrams (CMD) of the stellar groups. However, even with the excellent indicated spatial resolution, the blending of several stars in crowded fields can change the shape of the CMDs. Some of the blendings could be handled in the cases they produce particular features on the stellar PSF profile (e.g. abnormal sharpness, roundness, etc). But in some cases, the blend could be difficult to detect, this is the case, were a pair or several stars are in the same line of sight (e.g. observed in the same pixel). In this work, we investigated the importance of the blending effect in several crowded regions, using both numerical simulations and real ACS/HST data. In particular, we evaluated the influence of this effect over the CMDs, luminosity functions (LFs) and reddening estimations obtained from the observations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.10989v1-abstract-full').style.display = 'none'; document.getElementById('1903.10989v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 March, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">The 28th annual international Astronomical Data Analysis Software & Systems (ADASS, 2018)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1806.06841">arXiv:1806.06841</a> <span> [<a href="https://arxiv.org/pdf/1806.06841">pdf</a>, <a href="https://arxiv.org/format/1806.06841">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/sty1561">10.1093/mnras/sty1561 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Identification and analysis of the young population in the starburst galaxy NGC 253 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rodr%C3%ADguez%2C+M+J">M. J. Rodr铆guez</a>, <a href="/search/astro-ph?searchtype=author&query=Baume%2C+G">G. Baume</a>, <a href="/search/astro-ph?searchtype=author&query=Feinstein%2C+C">C. Feinstein</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="1806.06841v1-abstract-short" style="display: inline;"> We present a study of the young population in the starburst galaxy NGC 253. In particular, we focused our attention on searching young star groups, obtaining their main properties and studying their hierarchical organization. For this task, we used multiband images and their corresponding photometric data obtained with the Advanced Camera for Surveys of the Hubble Space Telescope (ACS/HST). We h… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.06841v1-abstract-full').style.display = 'inline'; document.getElementById('1806.06841v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1806.06841v1-abstract-full" style="display: none;"> We present a study of the young population in the starburst galaxy NGC 253. In particular, we focused our attention on searching young star groups, obtaining their main properties and studying their hierarchical organization. For this task, we used multiband images and their corresponding photometric data obtained with the Advanced Camera for Surveys of the Hubble Space Telescope (ACS/HST). We have first derived the absorption affecting the different regions of the galaxy. Then, we applied an automatic and objective searching method over the corrected data in order to detect young star groups. We complemented this result with the construction of the stellar density map for the blue young population. A statistical procedure to decontaminate the photometric diagrams from field stars was applied over the detected groups and we estimated their fundamental parameters. As a result, we built a catalog of 875 new identified young groups with their main characteristics, including coordinates, sizes, estimated number of members, stellar densities, luminosity function (LF) slopes and galactocentric distances. We observed these groups delineate different structures of the galaxy, and they are the last step in the hierarchical way in which the young population is organized. From their size distribution, we found they have typical radius of $\sim 40 - 50$ pc. These values are consistent with those ones found in others nearby galaxies. We estimated a mean value of the LF slope of 0.21 and an average density of 0.0006 stars/pc$^3$ for the identified young groups taking into account stars earlier than B6. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.06841v1-abstract-full').style.display = 'none'; document.getElementById('1806.06841v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 June, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">13 pages, 16 figures. This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society (MNRAS), Published by Oxford University Press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1510.06979">arXiv:1510.06979</a> <span> [<a href="https://arxiv.org/pdf/1510.06979">pdf</a>, <a href="https://arxiv.org/format/1510.06979">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/10.1093/mnras/stv2489">10.1093/mnras/stv2489 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The fingerprints of Photoionization and Shock-Ionization in two CSS sources </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Reynaldi%2C+V">V. Reynaldi</a>, <a href="/search/astro-ph?searchtype=author&query=Feinstein%2C+C">C. Feinstein</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="1510.06979v1-abstract-short" style="display: inline;"> We investigate the ionization state of the Extended Emission-Line Regions (EELRs) around two compact steep-spectrum (CSS) radio galaxies, 3C~268.3 and 3C~303.1, in order to identify the contribution of photoionization and shock-ionization. We perform a new spectroscopical (long-slit) analysis with GMOS/Gemini with the slit oriented in the radio-jet direction, where outflows are known to exist. The… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1510.06979v1-abstract-full').style.display = 'inline'; document.getElementById('1510.06979v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1510.06979v1-abstract-full" style="display: none;"> We investigate the ionization state of the Extended Emission-Line Regions (EELRs) around two compact steep-spectrum (CSS) radio galaxies, 3C~268.3 and 3C~303.1, in order to identify the contribution of photoionization and shock-ionization. We perform a new spectroscopical (long-slit) analysis with GMOS/Gemini with the slit oriented in the radio-jet direction, where outflows are known to exist. The [Ne V]$位3426$ emission is the most interesting feature of the spectra and the key to breaking the degeneracy between the models: since this emission-line is more extended than HeII, it challenges the ionization structure proposed by any photoionization model, also its intensity relative to H$尾$ does not behave as expected with respect to the ionization parameter U in the same scenario. On the contrary, when it is compared to the intensity of [OII]$\lambda3727$/H$尾$ and all these results are joined, the whole scenario is plausible to be explained as emission coming from the hot, compressed, shocked gas in shock-ionization models. Although the model fitting is strongly sensitive to the chosen line-ratios, it argues for the presence of external and strong ionizing fields, such as the precursor field created by the shock or/and the AGN radiation field. In this paper, we show how AGN photoionization and shock-ionization triggered by jet-cloud interaction work together in these EELRs in order to explain the observed trends and line-ratio behaviours in a kinematically acceptable way. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1510.06979v1-abstract-full').style.display = 'none'; document.getElementById('1510.06979v1-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">14 pages, 6 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/1406.3241">arXiv:1406.3241</a> <span> [<a href="https://arxiv.org/pdf/1406.3241">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"> VISTA Variables in the V铆a L谩ctea (VVV): Halfway Status and Results </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=Minniti%2C+D">Dante Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%A9k%C3%A1ny%2C+I">Istv谩n D茅k谩ny</a>, <a href="/search/astro-ph?searchtype=author&query=Saito%2C+R+K">Roberto K. Saito</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+P+W">Philip W. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=Emerson%2C+J">Jim Emerson</a>, <a href="/search/astro-ph?searchtype=author&query=Ahumada%2C+A+V">Andrea V. Ahumada</a>, <a href="/search/astro-ph?searchtype=author&query=Aigrain%2C+S">Suzanne Aigrain</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso%2C+M+V">Maria Victoria Alonso</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=Am%C3%B4res%2C+E+B">Eduardo B. Am么res</a>, <a href="/search/astro-ph?searchtype=author&query=Angeloni%2C+R">Rodolfo Angeloni</a>, <a href="/search/astro-ph?searchtype=author&query=Arias%2C+J">Julia Arias</a>, <a href="/search/astro-ph?searchtype=author&query=Bandyopadhyay%2C+R">Reba Bandyopadhyay</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">Rodolfo H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">Beatriz Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=Baume%2C+G">Gustavo Baume</a>, <a href="/search/astro-ph?searchtype=author&query=Beamin%2C+J+C">Juan Carlos Beamin</a>, <a href="/search/astro-ph?searchtype=author&query=Bedin%2C+L">Luigi Bedin</a>, <a href="/search/astro-ph?searchtype=author&query=Bica%2C+E">Eduardo Bica</a>, <a href="/search/astro-ph?searchtype=author&query=Borissova%2C+J">Jordanka Borissova</a>, <a href="/search/astro-ph?searchtype=author&query=Bronfman%2C+L">Leonardo Bronfman</a>, <a href="/search/astro-ph?searchtype=author&query=Carraro%2C+G">Giovanni Carraro</a>, <a href="/search/astro-ph?searchtype=author&query=Catelan%2C+M">M谩rcio Catelan</a>, <a href="/search/astro-ph?searchtype=author&query=Clari%C3%A1%2C+J+J">Juan J. Clari谩</a> , et al. (67 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="1406.3241v1-abstract-short" style="display: inline;"> The VISTA Variables in the V铆a L谩ctea (VVV) survey is one of six public ESO surveys, and is now in its 4th year of observing. Although far from being complete, the VVV survey has already delivered many results, some directly connected to the intended science goals (detection of variables stars, microlensing events, new star clusters), others concerning more exotic objects, e.g. novae. Now, at the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1406.3241v1-abstract-full').style.display = 'inline'; document.getElementById('1406.3241v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1406.3241v1-abstract-full" style="display: none;"> The VISTA Variables in the V铆a L谩ctea (VVV) survey is one of six public ESO surveys, and is now in its 4th year of observing. Although far from being complete, the VVV survey has already delivered many results, some directly connected to the intended science goals (detection of variables stars, microlensing events, new star clusters), others concerning more exotic objects, e.g. novae. Now, at the end of the fourth observing period, and comprising roughly 50% of the proposed observations, the actual status of the survey, as well some of the results based on the VVV data, are presented. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1406.3241v1-abstract-full').style.display = 'none'; document.getElementById('1406.3241v1-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 June, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">5 pages, 7 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ESO Messenger 155, (2014), 29-32 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1307.7489">arXiv:1307.7489</a> <span> [<a href="https://arxiv.org/pdf/1307.7489">pdf</a>, <a href="https://arxiv.org/ps/1307.7489">ps</a>, <a href="https://arxiv.org/format/1307.7489">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</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/stt1377">10.1093/mnras/stt1377 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Shock-ionization in the Extended Emission-Line Region of 3C~305. The last piece of the (optical) puzzle </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Reynaldi%2C+V">Victoria Reynaldi</a>, <a href="/search/astro-ph?searchtype=author&query=Feinstein%2C+C">Carlos Feinstein</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="1307.7489v1-abstract-short" style="display: inline;"> We present new Gemini spectroscopical data of the Extended Emission-Line Region of 3C~305 radio galaxy in order to achieve the final answer of the long-standing question about the ionizing mechanism. The spectra show strong kinematic disturbances within the most intense line-emitting region. The relative intensities amongst the emission lines agree with the gas being shocked during the interaction… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1307.7489v1-abstract-full').style.display = 'inline'; document.getElementById('1307.7489v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1307.7489v1-abstract-full" style="display: none;"> We present new Gemini spectroscopical data of the Extended Emission-Line Region of 3C~305 radio galaxy in order to achieve the final answer of the long-standing question about the ionizing mechanism. The spectra show strong kinematic disturbances within the most intense line-emitting region. The relative intensities amongst the emission lines agree with the gas being shocked during the interaction of the powerful radio jets with the ambient medium. The emission from the recombination region acts as a very effective cooling mechanism, which is supported by the presence of a neutral outflow. However, the observed intensity is almost an order of magnitude lower than expected in a pure shock model. So auto-ionizing shock models, in low-density and low-abundance regime, are required in order to account for the observed emission within the region. This scenario also supports the hypothesis that the optical emitting gas and the X-ray plasma are in pressure balance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1307.7489v1-abstract-full').style.display = 'none'; document.getElementById('1307.7489v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 July, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">13 pages, 6 figures. To be 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/1301.2216">arXiv:1301.2216</a> <span> [<a href="https://arxiv.org/pdf/1301.2216">pdf</a>, <a href="https://arxiv.org/ps/1301.2216">ps</a>, <a href="https://arxiv.org/format/1301.2216">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/stt042">10.1093/mnras/stt042 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Searching for evidence of jet-cloud interaction in radio galaxies. First results for 3C 381 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Reynaldi%2C+V">V. Reynaldi</a>, <a href="/search/astro-ph?searchtype=author&query=Feinstein%2C+C">C. Feinstein</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="1301.2216v1-abstract-short" style="display: inline;"> We present results of Gemini spectroscopy and Hubble Space Telescope imaging of the 3C~381 radio galaxy. Possible ionising mechanisms for the Extended Emission-Line Region were studied through state-of-the-art diagnostic analysis employing line-ratios. Photoionisation from the central engine as well as mixed-medium photoionisation models fail in reproducing both the strengths and the behaviour of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1301.2216v1-abstract-full').style.display = 'inline'; document.getElementById('1301.2216v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1301.2216v1-abstract-full" style="display: none;"> We present results of Gemini spectroscopy and Hubble Space Telescope imaging of the 3C~381 radio galaxy. Possible ionising mechanisms for the Extended Emission-Line Region were studied through state-of-the-art diagnostic analysis employing line-ratios. Photoionisation from the central engine as well as mixed-medium photoionisation models fail in reproducing both the strengths and the behaviour of the highest-excitation lines, such as [NeV]3424, HeII, and [OIII}]5007, which are measured at very large distances from the AGN. Shock-ionisation models provide a better fit to the observation. Expanding shocks with velocities higher than 500 km/s are capable of reaching the observed intensity ratios for lines with different ionisation states and excitation degrees. This model also provide a direct explanation of the mechanical energy input needed to explain the high-velocity line-splitting observed in the velocity field. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1301.2216v1-abstract-full').style.display = 'none'; document.getElementById('1301.2216v1-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, 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">21 pages, 11 figures; to be published in 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/1211.2801">arXiv:1211.2801</a> <span> [<a href="https://arxiv.org/pdf/1211.2801">pdf</a>, <a href="https://arxiv.org/ps/1211.2801">ps</a>, <a href="https://arxiv.org/format/1211.2801">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201220107">10.1051/0004-6361/201220107 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Massive open star clusters using the VVV survey II. Discovery of six clusters with Wolf-Rayet stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chen%C3%A9%2C+A+-">A. -N. Chen茅</a>, <a href="/search/astro-ph?searchtype=author&query=Borissova%2C+J">J. Borissova</a>, <a href="/search/astro-ph?searchtype=author&query=Bonatto%2C+C">C. Bonatto</a>, <a href="/search/astro-ph?searchtype=author&query=Majaess%2C+D+J">D. J. Majaess</a>, <a href="/search/astro-ph?searchtype=author&query=Baume%2C+G">G. Baume</a>, <a href="/search/astro-ph?searchtype=author&query=Clarke%2C+J+R+A">J. R. A. Clarke</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtev%2C+R">R. Kurtev</a>, <a href="/search/astro-ph?searchtype=author&query=Schnurr%2C+O">O. Schnurr</a>, <a href="/search/astro-ph?searchtype=author&query=Bouret%2C+J+-">J. -C. Bouret</a>, <a href="/search/astro-ph?searchtype=author&query=Catelan%2C+M">M. Catelan</a>, <a href="/search/astro-ph?searchtype=author&query=Emerson%2C+J+P">J. P. Emerson</a>, <a href="/search/astro-ph?searchtype=author&query=Feinstein%2C+C">C. Feinstein</a>, <a href="/search/astro-ph?searchtype=author&query=Geisler%2C+D">D. Geisler</a>, <a href="/search/astro-ph?searchtype=author&query=de+Grijs%2C+R">R. de Grijs</a>, <a href="/search/astro-ph?searchtype=author&query=Herv%C3%A9%2C+A">A. Herv茅</a>, <a href="/search/astro-ph?searchtype=author&query=Ivanov%2C+V+D">V. D. Ivanov</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+M+S+N">M. S. N. Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+P">P. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=Mahy%2C+L">L. Mahy</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+F">F. Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Mauro%2C+F">F. Mauro</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Bidin%2C+C+M">C. Moni Bidin</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="1211.2801v1-abstract-short" style="display: inline;"> Context: The ESO Public Survey "VISTA Variables in the V铆a L谩ctea" (VVV) provides deep multi-epoch infrared observations for an unprecedented 562 sq. degrees of the Galactic bulge, and adjacent regions of the disk. In this survey nearly 150 new open clusters and cluster candidates have been discovered. Aims: This is the second in a series of papers about young, massive open clusters observed using… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1211.2801v1-abstract-full').style.display = 'inline'; document.getElementById('1211.2801v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1211.2801v1-abstract-full" style="display: none;"> Context: The ESO Public Survey "VISTA Variables in the V铆a L谩ctea" (VVV) provides deep multi-epoch infrared observations for an unprecedented 562 sq. degrees of the Galactic bulge, and adjacent regions of the disk. In this survey nearly 150 new open clusters and cluster candidates have been discovered. Aims: This is the second in a series of papers about young, massive open clusters observed using the VVV survey. We present the first study of six recently discovered clusters. These clusters contain at least one newly discovered Wolf-Rayet (WR) star. Methods: Following the methodology presented in the first paper of the series, wide-field, deep JHKs VVV observations, combined with new infrared spectroscopy, are employed to constrain fundamental parameters for a subset of clusters. Results: We affirm that the six studied stellar groups are real young (2-7 Myr) and massive (between 0.8 and 2.2 10^3 Msol) clusters. They are highly obscured (Av ~ 5-24 mag) and compact (1-2 pc). In addition to WR stars, two of the six clusters also contain at least one red supergiant star. We claim the discovery of 8 new WR stars, and 3 stars showing WR-like emission lines which could be classified WR or OIf. Preliminary analysis provides initial masses of ~30-50 Msol for the WR stars. Finally,we discuss the spiral structure of the Galaxy using as tracers the six new clusters together with the previously studied VVV clusters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1211.2801v1-abstract-full').style.display = 'none'; document.getElementById('1211.2801v1-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 November, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 8 figurs, accepted in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1206.6104">arXiv:1206.6104</a> <span> [<a href="https://arxiv.org/pdf/1206.6104">pdf</a>, <a href="https://arxiv.org/ps/1206.6104">ps</a>, <a href="https://arxiv.org/format/1206.6104">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201219064">10.1051/0004-6361/201219064 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Massive open star clusters using the VVV survey I. Presentation of the data and description of the approach </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chen%C3%A9%2C+A+-">A. -N. Chen茅</a>, <a href="/search/astro-ph?searchtype=author&query=Borissova%2C+J">J. Borissova</a>, <a href="/search/astro-ph?searchtype=author&query=Clarke%2C+J+R+A">J. R. A. Clarke</a>, <a href="/search/astro-ph?searchtype=author&query=Bonatto%2C+C">C. Bonatto</a>, <a href="/search/astro-ph?searchtype=author&query=Majaess%2C+D+J">D. J. Majaess</a>, <a href="/search/astro-ph?searchtype=author&query=Bidin%2C+C+M">C. Moni Bidin</a>, <a href="/search/astro-ph?searchtype=author&query=Sale%2C+S+E">S. E. Sale</a>, <a href="/search/astro-ph?searchtype=author&query=Mauro%2C+F">F. Mauro</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtev%2C+R">R. Kurtev</a>, <a href="/search/astro-ph?searchtype=author&query=Baume%2C+G">G. Baume</a>, <a href="/search/astro-ph?searchtype=author&query=Feinstein%2C+C">C. Feinstein</a>, <a href="/search/astro-ph?searchtype=author&query=Ivanov%2C+V+D">V. D. Ivanov</a>, <a href="/search/astro-ph?searchtype=author&query=Geisler%2C+D">D. Geisler</a>, <a href="/search/astro-ph?searchtype=author&query=Catelan%2C+M">M. Catelan</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+P">P. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=de+Grijs%2C+R">R. de Grijs</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+M+S+N">M. S. N. Kumar</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="1206.6104v2-abstract-short" style="display: inline;"> Context: The ESO Public Survey "VISTA Variables in the V铆a L谩ctea" (VVV) provides deep multi-epoch infrared observations for an unprecedented 562 sq. degrees of the Galactic bulge, and adjacent regions of the disk. Aims: The VVV observations will foster the construction of a sample of Galactic star clusters with reliable and homogeneously derived physical parameters (e.g., age, distance, and mass,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1206.6104v2-abstract-full').style.display = 'inline'; document.getElementById('1206.6104v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1206.6104v2-abstract-full" style="display: none;"> Context: The ESO Public Survey "VISTA Variables in the V铆a L谩ctea" (VVV) provides deep multi-epoch infrared observations for an unprecedented 562 sq. degrees of the Galactic bulge, and adjacent regions of the disk. Aims: The VVV observations will foster the construction of a sample of Galactic star clusters with reliable and homogeneously derived physical parameters (e.g., age, distance, and mass, etc.). In this first paper in a series, the methodology employed to establish cluster parameters for the envisioned database are elaborated upon by analyzing a subsample of 4 known young open clusters: Danks 1, Danks 2, RCW 79, and DBS 132. The analysis offers a first glimpse of the information that can be gleaned for the final cluster database from the VVV observations. Methods: Wide-field, deep JHKs VVV observations, combined with new infrared spectroscopy, are employed to constrain fundamental parameters for a subset of clusters. Results: Results inferred from the deep near-infrared photometry which features mitigated uncertainties (e.g. the accuracy of the photometry is better than 0.1mag for Ks<18mag), the wide field-of-view of the VVV survey, and numerous high quality low resolution spectra (typically more than 10 per cluster), are used to establish independent cluster parameters which enable existing determinations to be assessed. An anomalous reddening law in the direction toward the Danks' clusters is found, i.e. E(J-H)/E(H-Ks)=2.20+/-0.06, which exceeds published values for the inner Galaxy. The G305 star forming complex, which includes the Danks' clusters, lies beyond the Sagittarius-Carina spiral arm and occupies the Centaurus arm. Finally, the first deep infrared color-magnitude diagram of RCW 79 is presented which reveal a sizable pre-main sequence population. A list of candidate variable stars in G305 region is reported. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1206.6104v2-abstract-full').style.display = 'none'; document.getElementById('1206.6104v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 July, 2012; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 June, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 13 figures, 4 tables, 3 tables in the online material, photometric Catalogs to be published soon. Accepted in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1111.5511">arXiv:1111.5511</a> <span> [<a href="https://arxiv.org/pdf/1111.5511">pdf</a>, <a href="https://arxiv.org/ps/1111.5511">ps</a>, <a href="https://arxiv.org/format/1111.5511">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201118407">10.1051/0004-6361/201118407 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> VVV DR1: The First Data Release of the Milky Way Bulge and Southern Plane from the Near-Infrared ESO Public Survey VISTA Variables in the Via Lactea </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Saito%2C+R+K">R. K. Saito</a>, <a href="/search/astro-ph?searchtype=author&query=Hempel%2C+M">M. Hempel</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+P+W">P. W. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">M. Rejkuba</a>, <a href="/search/astro-ph?searchtype=author&query=Toledo%2C+I">I. Toledo</a>, <a href="/search/astro-ph?searchtype=author&query=Gonzalez%2C+O+A">O. A. Gonzalez</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso-Garcia%2C+J">J. Alonso-Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Irwin%2C+M+J">M. J. Irwin</a>, <a href="/search/astro-ph?searchtype=author&query=Gonzalez-Solares%2C+E">E. Gonzalez-Solares</a>, <a href="/search/astro-ph?searchtype=author&query=Hodgkin%2C+S+T">S. T. Hodgkin</a>, <a href="/search/astro-ph?searchtype=author&query=Lewis%2C+J+R">J. R. Lewis</a>, <a href="/search/astro-ph?searchtype=author&query=Cross%2C+N">N. Cross</a>, <a href="/search/astro-ph?searchtype=author&query=Ivanov%2C+V+D">V. D. Ivanov</a>, <a href="/search/astro-ph?searchtype=author&query=Kerins%2C+E">E. Kerins</a>, <a href="/search/astro-ph?searchtype=author&query=Emerson%2C+J+P">J. P. Emerson</a>, <a href="/search/astro-ph?searchtype=author&query=Soto%2C+M">M. Soto</a>, <a href="/search/astro-ph?searchtype=author&query=Amores%2C+E+B">E. B. Amores</a>, <a href="/search/astro-ph?searchtype=author&query=Gurovich%2C+S">S. Gurovich</a>, <a href="/search/astro-ph?searchtype=author&query=Dekany%2C+I">I. Dekany</a>, <a href="/search/astro-ph?searchtype=author&query=Angeloni%2C+R">R. Angeloni</a>, <a href="/search/astro-ph?searchtype=author&query=Beamin%2C+J+C">J. C. Beamin</a>, <a href="/search/astro-ph?searchtype=author&query=Catelan%2C+M">M. Catelan</a>, <a href="/search/astro-ph?searchtype=author&query=Padilla%2C+N">N. Padilla</a>, <a href="/search/astro-ph?searchtype=author&query=Zoccali%2C+M">M. Zoccali</a> , et al. (85 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="1111.5511v1-abstract-short" style="display: inline;"> The ESO Public Survey VISTA Variables in the Via Lactea (VVV) started in 2010. VVV targets 562 sq. deg in the Galactic bulge and an adjacent plane region and is expected to run for ~5 years. In this paper we describe the progress of the survey observations in the first observing season, the observing strategy and quality of the data obtained. The observations are carried out on the 4-m VISTA teles… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1111.5511v1-abstract-full').style.display = 'inline'; document.getElementById('1111.5511v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1111.5511v1-abstract-full" style="display: none;"> The ESO Public Survey VISTA Variables in the Via Lactea (VVV) started in 2010. VVV targets 562 sq. deg in the Galactic bulge and an adjacent plane region and is expected to run for ~5 years. In this paper we describe the progress of the survey observations in the first observing season, the observing strategy and quality of the data obtained. The observations are carried out on the 4-m VISTA telescope in the ZYJHKs filters. In addition to the multi-band imaging the variability monitoring campaign in the Ks filter has started. Data reduction is carried out using the pipeline at the Cambridge Astronomical Survey Unit. The photometric and astrometric calibration is performed via the numerous 2MASS sources observed in each pointing. The first data release contains the aperture photometry and astrometric catalogues for 348 individual pointings in the ZYJHKs filters taken in the 2010 observing season. The typical image quality is ~0.9-1.0". The stringent photometric and image quality requirements of the survey are satisfied in 100% of the JHKs images in the disk area and 90% of the JHKs images in the bulge area. The completeness in the Z and Y images is 84% in the disk, and 40% in the bulge. The first season catalogues contain 1.28x10^8 stellar sources in the bulge and 1.68x10^8 in the disk area detected in at least one of the photometric bands. The combined, multi-band catalogues contain more than 1.63x10^8 stellar sources. About 10% of these are double detections due to overlapping adjacent pointings. These overlapping multiple detections are used to characterise the quality of the data. The images in the JHKs bands extend typically ~4 mag deeper than 2MASS. The magnitude limit and photometric quality depend strongly on crowding in the inner Galactic regions. The astrometry for Ks=15-18 mag has rms ~35-175 mas. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1111.5511v1-abstract-full').style.display = 'none'; document.getElementById('1111.5511v1-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 November, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2011. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astronomy and Astrophysics (Section 14: Catalogs and data)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1003.2985">arXiv:1003.2985</a> <span> [<a href="https://arxiv.org/pdf/1003.2985">pdf</a>, <a href="https://arxiv.org/ps/1003.2985">ps</a>, <a href="https://arxiv.org/format/1003.2985">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/200913171">10.1051/0004-6361/200913171 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Polarimetry of an Intermediate-age Open Cluster: NGC 5617 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Orsatti%2C+A+M">Ana Maria Orsatti</a>, <a href="/search/astro-ph?searchtype=author&query=Feinstein%2C+C">Carlos Feinstein</a>, <a href="/search/astro-ph?searchtype=author&query=Vergne%2C+M+M">M. Marcela Vergne</a>, <a href="/search/astro-ph?searchtype=author&query=Martinez%2C+R+E">Ruben E. Martinez</a>, <a href="/search/astro-ph?searchtype=author&query=Vega%2C+E+I">E. Irene Vega</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="1003.2985v1-abstract-short" style="display: inline;"> We present polarimetric observations in the UBVRI bands of 72 stars located in the direction of the medium age open cluster NGC 5617. Our intention is to use polarimetry as a tool membership identification, by building on previous investigations intended mainly to determine the cluster's general characteristics rather than provide membership suitable for studies such as stellar content and metalli… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1003.2985v1-abstract-full').style.display = 'inline'; document.getElementById('1003.2985v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1003.2985v1-abstract-full" style="display: none;"> We present polarimetric observations in the UBVRI bands of 72 stars located in the direction of the medium age open cluster NGC 5617. Our intention is to use polarimetry as a tool membership identification, by building on previous investigations intended mainly to determine the cluster's general characteristics rather than provide membership suitable for studies such as stellar content and metallicity, as well as study the characteristics of the dust lying between the Sun and the cluster. The obsevations were carried out using the five-channel photopolarimeter of the Torino Astronomical Observatory attached to the 2.15m telescope at the Complejo Astron贸mico El Leoncito (CASLEO; Argentina. We are able to add 32 stars to the list of members of NGC 5617, and review the situation for others listed in the literature. In particular, we find that five blue straggler stars in the region of the cluster are located behind the same dust as the member stars are and we confirm the membership of two red giants. The proposed polarimetric memberships are compared with those derived by photometric and kinematical methods, with excellent results. Among the observed stars, we identify 10 with intrinsic polarization in their light. NGC 5617 can be polarimetrically characterized with $P_{max}= 4.40%$ and $ 胃_{v}= 73^\circ.1$. The spread in polarization values for the stars observed in the direction of the cluster seems to be caused by the uneven distribution of dust in front of the cluster's face. Finally, we find that in the direction of the cluster, the interstellar medium is apparently free of dust, from the Sun's position up to the Carina-Sagittarius arm, where NGC 5617 seems to be located at its farthest border. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1003.2985v1-abstract-full').style.display = 'none'; document.getElementById('1003.2985v1-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 March, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2010. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1003.1250">arXiv:1003.1250</a> <span> [<a href="https://arxiv.org/pdf/1003.1250">pdf</a>, <a href="https://arxiv.org/ps/1003.1250">ps</a>, <a href="https://arxiv.org/format/1003.1250">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/10.1111/j.1365-2966.2010.16242.x">10.1111/j.1365-2966.2010.16242.x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Optical polarization observations in the Scorpius region: NGC 6124 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vergne%2C+M+M">M. Marcela Vergne</a>, <a href="/search/astro-ph?searchtype=author&query=Feinstein%2C+C">Carlos Feinstein</a>, <a href="/search/astro-ph?searchtype=author&query=Martinez%2C+R">Ruben Martinez</a>, <a href="/search/astro-ph?searchtype=author&query=Orsatti%2C+A+M">Ana Maria Orsatti</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez%2C+M+P">Maria Paula Alvarez</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="1003.1250v1-abstract-short" style="display: inline;"> We have obtained optical multicolour (UBVRI) linear polarimetric data for 46 of the brightest stars in the area of the open cluster NGC 6124 in order to investigate the properties of the interstellar medium (ISM) that lies along the line of sight toward the cluster. Our data yield a mean polarization efficiency of $P_V/E_{B-V}=3.1\pm$0.62, i.e., a value lower than the polarization produced by th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1003.1250v1-abstract-full').style.display = 'inline'; document.getElementById('1003.1250v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1003.1250v1-abstract-full" style="display: none;"> We have obtained optical multicolour (UBVRI) linear polarimetric data for 46 of the brightest stars in the area of the open cluster NGC 6124 in order to investigate the properties of the interstellar medium (ISM) that lies along the line of sight toward the cluster. Our data yield a mean polarization efficiency of $P_V/E_{B-V}=3.1\pm$0.62, i.e., a value lower than the polarization produced by the ISM with normal efficiency for an average color excess of $E_{B-V}=0.80$ as that found for NGC 6124. Besides, the polarization shows an orientation of $胃\sim 8^\circ$.1 which is not parallel to the Galactic Disk,an effect that we think may be caused by the Lupus Cloud. Our analysis also indicates that the observed visual extinction in NGC 6124 is caused by the presence of three different absorption sheets located between the Sun and NGC 6124. The values of the internal dispersion of the polarization ($螖P_V\sim 1.3% $) and of the colour excess ($螖E_{B-V}\sim 0.29$ mag) for the members of NGC 6124 seem to be compatible with the presence of an intra-cluster dust component. Only six stars exhibit some evidence of intrinsic polarization.Our work also shows that polarimetry provides an excellent tool to distinguish between member and non-member stars of a cluster. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1003.1250v1-abstract-full').style.display = 'none'; document.getElementById('1003.1250v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 March, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2010. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0912.1056">arXiv:0912.1056</a> <span> [<a href="https://arxiv.org/pdf/0912.1056">pdf</a>, <a href="https://arxiv.org/ps/0912.1056">ps</a>, <a href="https://arxiv.org/format/0912.1056">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/10.1016/j.newast.2009.12.002">10.1016/j.newast.2009.12.002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> VISTA Variables in the Via Lactea (VVV): The public ESO near-IR variability survey of the Milky Way </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+P+W">P. W. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=Emerson%2C+J+P">J. P. Emerson</a>, <a href="/search/astro-ph?searchtype=author&query=Saito%2C+R+K">R. K. Saito</a>, <a href="/search/astro-ph?searchtype=author&query=Hempel%2C+M">M. Hempel</a>, <a href="/search/astro-ph?searchtype=author&query=Pietrukowicz%2C+P">P. Pietrukowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Ahumada%2C+A+V">A. V. Ahumada</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso%2C+M+V">M. V. Alonso</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso-Garc%C3%ADa%2C+J">J. Alonso-Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Arias%2C+J+I">J. I. Arias</a>, <a href="/search/astro-ph?searchtype=author&query=Bandyopadhyay%2C+R+M">R. M. Bandyopadhyay</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">R. H. Barb谩</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=Bica%2C+E">E. Bica</a>, <a href="/search/astro-ph?searchtype=author&query=Borissova%2C+J">J. Borissova</a>, <a href="/search/astro-ph?searchtype=author&query=Bronfman%2C+L">L. Bronfman</a>, <a href="/search/astro-ph?searchtype=author&query=Carraro%2C+G">G. Carraro</a>, <a href="/search/astro-ph?searchtype=author&query=Catelan%2C+M">M. Catelan</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=Cross%2C+N">N. Cross</a>, <a href="/search/astro-ph?searchtype=author&query=de+Grijs%2C+R">R. de Grijs</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%A9k%C3%A1ny%2C+I">I. D茅k谩ny</a>, <a href="/search/astro-ph?searchtype=author&query=Drew%2C+J+E">J. E. Drew</a>, <a href="/search/astro-ph?searchtype=author&query=Fari%C3%B1a%2C+C">C. Fari帽a</a> , et al. (41 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="0912.1056v2-abstract-short" style="display: inline;"> We describe the public ESO near-IR variability survey (VVV) scanning the Milky Way bulge and an adjacent section of the mid-plane where star formation activity is high. The survey will take 1929 hours of observations with the 4-metre VISTA telescope during five years (2010-2014), covering ~10^9 point sources across an area of 520 deg^2, including 33 known globular clusters and ~350 open clusters… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0912.1056v2-abstract-full').style.display = 'inline'; document.getElementById('0912.1056v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0912.1056v2-abstract-full" style="display: none;"> We describe the public ESO near-IR variability survey (VVV) scanning the Milky Way bulge and an adjacent section of the mid-plane where star formation activity is high. The survey will take 1929 hours of observations with the 4-metre VISTA telescope during five years (2010-2014), covering ~10^9 point sources across an area of 520 deg^2, including 33 known globular clusters and ~350 open clusters. The final product will be a deep near-IR atlas in five passbands (0.9-2.5 microns) and a catalogue of more than 10^6 variable point sources. Unlike single-epoch surveys that, in most cases, only produce 2-D maps, the VVV variable star survey will enable the construction of a 3-D map of the surveyed region using well-understood distance indicators such as RR Lyrae stars, and Cepheids. It will yield important information on the ages of the populations. The observations will be combined with data from MACHO, OGLE, EROS, VST, Spitzer, HST, Chandra, INTEGRAL, WISE, Fermi LAT, XMM-Newton, GAIA and ALMA for a complete understanding of the variable sources in the inner Milky Way. This public survey will provide data available to the whole community and therefore will enable further studies of the history of the Milky Way, its globular cluster evolution, and the population census of the Galactic Bulge and center, as well as the investigations of the star forming regions in the disk. The combined variable star catalogues will have important implications for theoretical investigations of pulsation properties of stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0912.1056v2-abstract-full').style.display = 'none'; document.getElementById('0912.1056v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 December, 2009; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 December, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2009. </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 New Astronomy</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> New Astron.15:433-443,2010 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0311133">arXiv:astro-ph/0311133</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0311133">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0311133">ps</a>, <a href="https://arxiv.org/format/astro-ph/0311133">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/378799">10.1086/378799 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Optical polarization observations of NGC 6231: evidence for a past SN fingerprint </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Feinstein%2C+C">Carlos Feinstein</a>, <a href="/search/astro-ph?searchtype=author&query=Martinez%2C+R">Ruben Martinez</a>, <a href="/search/astro-ph?searchtype=author&query=Vergne%2C+M+M">M. Marcela Vergne</a>, <a href="/search/astro-ph?searchtype=author&query=Baume%2C+G">Gustavo Baume</a>, <a href="/search/astro-ph?searchtype=author&query=Vazquez%2C+R">Ruben Vazquez</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0311133v1-abstract-short" style="display: inline;"> We present the first linear multicolor polarization observations for a sample of 35 stars in the direction of the Galactic cluster NGC 6231. We have found a complex pattern in the angles of the polarimetric vectors. Near the core of this cluster the structure shows a semi-circular pattern that we have interpreted as a re-orientation of the dust particles, showing the morphology of the magnetic f… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0311133v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0311133v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0311133v1-abstract-full" style="display: none;"> We present the first linear multicolor polarization observations for a sample of 35 stars in the direction of the Galactic cluster NGC 6231. We have found a complex pattern in the angles of the polarimetric vectors. Near the core of this cluster the structure shows a semi-circular pattern that we have interpreted as a re-orientation of the dust particles, showing the morphology of the magnetic field. We propose that a supernova event has occurred some time ago and produced a shock on the local ISM. We discuss in this paper independent confirmations othis event, both from the studies on the diffuse interstellar absorptions Crawford (2001) and the results of the pre-main sequence stars (PMS) given by Sung et al. (1998). We also show that a supernova is supported by the evolutive status of the cluster. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0311133v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0311133v1-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 November, 2003; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2003. </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, 4 figures, ApJ Accepted</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J. 598 (2003) 349-356 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0110409">arXiv:astro-ph/0110409</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0110409">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0110409">ps</a>, <a href="https://arxiv.org/format/astro-ph/0110409">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/324604">10.1086/324604 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Filaments and Ionized Gas in the Vicinity of 3C 244.1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Feinstein%2C+C">Carlos Feinstein</a>, <a href="/search/astro-ph?searchtype=author&query=Macchetto%2C+F+D">F. Duccio Macchetto</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">Andre R. Martel</a>, <a href="/search/astro-ph?searchtype=author&query=Sparks%2C+W+B">William B. Sparks</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0110409v1-abstract-short" style="display: inline;"> We present results of Hubble Space Telescope observations of the radio galaxy 3C 244.1. The broadband F702W (R) and F555W (V) images (WFPC2/PC) show an elliptical galaxy and gaseous filaments and blobs surrounding it. In the narrow-band ramp filter, dominated by [OIII]lambda5007, these filaments are bright and have the same morphology as the broad band images. To the south, the filaments have a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0110409v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0110409v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0110409v1-abstract-full" style="display: none;"> We present results of Hubble Space Telescope observations of the radio galaxy 3C 244.1. The broadband F702W (R) and F555W (V) images (WFPC2/PC) show an elliptical galaxy and gaseous filaments and blobs surrounding it. In the narrow-band ramp filter, dominated by [OIII]lambda5007, these filaments are bright and have the same morphology as the broad band images. To the south, the filaments have a cone-shaped structure and the radio jet is located at the center of this cone. To the north of the galaxy, the structure is found near the nucleus of the galaxy within its elliptical profile. From the photometry, the two brighter structures seem to be extended narrow line emission regions (ENLRs). The comparison with diagnostic line ratios shows that the observed emission is consistent with interactions between the expanding radio-jet and the local denser medium. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0110409v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0110409v1-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 October, 2001; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2001. </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 and 3 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/astro-ph/0007093">arXiv:astro-ph/0007093</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0007093">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0007093">ps</a>, <a href="https://arxiv.org/format/astro-ph/0007093">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/301562">10.1086/301562 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The highly polarized open cluster Trumpler 27 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Feinstein%2C+C">Carlos Feinstein</a>, <a href="/search/astro-ph?searchtype=author&query=Baume%2C+G">Gustavo Baume</a>, <a href="/search/astro-ph?searchtype=author&query=Vazquez%2C+R">Ruben Vazquez</a>, <a href="/search/astro-ph?searchtype=author&query=Niemela%2C+V">Virpi Niemela</a>, <a href="/search/astro-ph?searchtype=author&query=Cerruti%2C+M+A">Miguel Angel Cerruti</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0007093v1-abstract-short" style="display: inline;"> We have carried out multicolor linear polarimetry (UBVRI) of the brightest stars in the area of the open cluster Trumpler 27. Our data show a high level of polarization in the stellar light with a considerable dispersion, from $P = 4%$ to $P = 9.5%$. The polarization vectors of the cluster members appear to be aligned. Foreground polarization was estimated from the data of some non-member object… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0007093v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0007093v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0007093v1-abstract-full" style="display: none;"> We have carried out multicolor linear polarimetry (UBVRI) of the brightest stars in the area of the open cluster Trumpler 27. Our data show a high level of polarization in the stellar light with a considerable dispersion, from $P = 4%$ to $P = 9.5%$. The polarization vectors of the cluster members appear to be aligned. Foreground polarization was estimated from the data of some non-member objects, for which two different components were resolved: the first one associated with a dust cloud close to the Sun producing $P_{位max}=1.3%$ and $胃=146$ degrees, and a second component, the main source of polarization for the cluster members, originated in another dust cloud, which polarizes the light in the direction of $胃= 29.5$ degrees. From a detailed analysis, we found that the two components have associated values $E_{B-V} < 0.45 $ for the first one, and $E_{B-V} > 0.75$ for the other. Due the difference in the orientation of both polarization vectors, almost 90 degrees (180 degrees at the Stokes representation), the first cloud ($胃\sim 146$ degrees) depolarize the light strongly polarized by the second one ($胃\sim 29.5$ degrees). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0007093v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0007093v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 July, 2000; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2000. </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, 6 Figures, 2 tables (9 Pages), 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/astro-ph/9906059">arXiv:astro-ph/9906059</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/9906059">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/9906059">ps</a>, <a href="https://arxiv.org/format/astro-ph/9906059">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/308030">10.1086/308030 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Extended Line Region of 3C 299 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Feinstein%2C+C">Carlos Feinstein</a>, <a href="/search/astro-ph?searchtype=author&query=Macchetto%2C+F+D">F. Duccio Macchetto</a>, <a href="/search/astro-ph?searchtype=author&query=Martel%2C+A+R">Andre R. Martel</a>, <a href="/search/astro-ph?searchtype=author&query=Sparks%2C+W+B">William B. Sparks</a>, <a href="/search/astro-ph?searchtype=author&query=McCarthy%2C+P+J">Patrick J. McCarthy</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/9906059v1-abstract-short" style="display: inline;"> We present results of HST observations of the radio galaxy 3C 299. The broad-band F702W (R) and F555W (V) images (WFPC2/PC) show an elliptical galaxy, with a comet-like structure extending to the NE in the radio jet direction. The [OIII]$位$5007 emission line map, shows a bi-conical structure centered on the nucleus, that overlaps the structure found in the broad-band filters. The radio core coin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9906059v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/9906059v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/9906059v1-abstract-full" style="display: none;"> We present results of HST observations of the radio galaxy 3C 299. The broad-band F702W (R) and F555W (V) images (WFPC2/PC) show an elliptical galaxy, with a comet-like structure extending to the NE in the radio jet direction. The [OIII]$位$5007 emission line map, shows a bi-conical structure centered on the nucleus, that overlaps the structure found in the broad-band filters. The radio core coincides with the center of the bi-conical structure and the radio axes are aligned with the direction of the cones. These data show clear evidence of a strong interaction between the radio jet and the NE morphology of the galaxy. We show evidence that this NE region is an ENLR; the line-ratio diagnostics show that models involving gas shocked by the radio-jet plus ionization from a precursor HII region, produced itself by the ionizing photons of the postshocked gas on the preshocked gas provide a good match to the observations. We investigate the spatial behavior of the ionizing parameter $U$, by determining the [OIII]/[OII] line ratio which is sensitive to the change of the ionization parameter, and trace its behavior over the ENLR along the radio jet direction. We find that [OIII]/[OII] does not follow a simple dilution model, but rather that it is approximately constant over a large range of distance from the nucleus thus requiring a local source of ionization which seems to be compatible with the shock models driven by the radio jet. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9906059v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/9906059v1-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 June, 1999; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 1999. </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, 9 Postscript figures, ApJ accepted, uses aaspp.sty</span> </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 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