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<button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Dekany%2C+I&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Dekany%2C+I&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Dekany%2C+I&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> </ul> </nav> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.03497">arXiv:2501.03497</a> <span> [<a href="https://arxiv.org/pdf/2501.03497">pdf</a>, <a href="https://arxiv.org/format/2501.03497">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 Galactic Bulge exploration IV.: RR~Lyrae stars as traces of the Galactic bar -- 3D and 5D analysis, extinction variation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Prudil%2C+Z">Z. Prudil</a>, <a href="/search/astro-ph?searchtype=author&query=Kunder%2C+A">A. Kunder</a>, <a href="/search/astro-ph?searchtype=author&query=Silva%2C+L+B+e">L. Beraldo e Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Gough-Kelly%2C+S">S. Gough-Kelly</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">M. Rejkuba</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+S+R">S. R. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Debattista%2C+V+P">V. P. Debattista</a>, <a href="/search/astro-ph?searchtype=author&query=Gerhard%2C+O">O. Gerhard</a>, <a href="/search/astro-ph?searchtype=author&query=Rich%2C+R+M">R. M. Rich</a>, <a href="/search/astro-ph?searchtype=author&query=Nataf%2C+D+M">D. M. Nataf</a>, <a href="/search/astro-ph?searchtype=author&query=Koch-Hansen%2C+A+J">A. J. Koch-Hansen</a>, <a href="/search/astro-ph?searchtype=author&query=Savino%2C+A">A. Savino</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%A9k%C3%A1ny%2C+I">I. D茅k谩ny</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2501.03497v1-abstract-short" style="display: inline;"> We created new reddening maps and derived new extinction laws from visual to near-infrared passbands using improved RR~Lyrae period-absolute magnitude-metallicity relations, thus enabling distance estimates for individual bulge RR~Lyrae variables. The extinction law is most uniform in RIK and RJK and the distances to individual RR~Lyrae based on these colors are determined with an accuracy six and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.03497v1-abstract-full').style.display = 'inline'; document.getElementById('2501.03497v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.03497v1-abstract-full" style="display: none;"> We created new reddening maps and derived new extinction laws from visual to near-infrared passbands using improved RR~Lyrae period-absolute magnitude-metallicity relations, thus enabling distance estimates for individual bulge RR~Lyrae variables. The extinction law is most uniform in RIK and RJK and the distances to individual RR~Lyrae based on these colors are determined with an accuracy six and four percent, respectively. Using only the near-infrared passbands for distance estimation we inferred the distance to the Galactic center equal to djk = 8.2 +- 0.001(stat) +- 0.53(sys)pc after geometrical correction. We show that variations in the extinction law toward the Galactic bulge can mimic a barred spatial distribution in the bulge RR~Lyrae star population in visual passbands. This arises from a gradient in extinction differences along Galactic longitudes and latitudes, which can create the perception of the Galactic bar, particularly when using visual passband-based distances. A barred angle in the RR~Lyrae spatial distribution disappears when near-infrared passband-based distances are used, as well as when reddening law variations are incorporated in visual passband-based distances. The prominence of the bar, as traced by RR~Lyrae stars, depends on their metallicity, with metal-poor RR~Lyrae stars ([Fe/H]<-1.0dex) showing little to no tilt with respect to the bar. Metal-rich ([Fe/H]>-1.0dex) RR~Lyrae stars do show a barred/bulge signature in spatial properties derived using near-infrared distances, with an angle 喂 = 18 +- 5deg, consistent with previous bar measurements from the literature. The 5D kinematic analysis, primarily based on transverse velocities, indicates a rotational lag in RR~Lyrae stars compared to red clump giants. Despite variations in the extinction law, our kinematic conclusions are robust across different distance estimation methods. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.03497v1-abstract-full').style.display = 'none'; document.getElementById('2501.03497v1-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 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">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/2404.05279">arXiv:2404.05279</a> <span> [<a href="https://arxiv.org/pdf/2404.05279">pdf</a>, <a href="https://arxiv.org/format/2404.05279">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> The Galactic bulge exploration II. Line-of-sight velocity templates for single-mode RR~Lyrae stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Prudil%2C+Z">Z. Prudil</a>, <a href="/search/astro-ph?searchtype=author&query=Smolec%2C+R">R. Smolec</a>, <a href="/search/astro-ph?searchtype=author&query=Kunder%2C+A">A. Kunder</a>, <a href="/search/astro-ph?searchtype=author&query=Koch-Hansen%2C+A+J">A. J Koch-Hansen</a>, <a href="/search/astro-ph?searchtype=author&query=Dekany%2C+I">I. Dekany</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.05279v2-abstract-short" style="display: inline;"> We present a new set of tools to derive systemic velocities for single-mode RR~Lyrae stars from visual and near-infrared spectra. We derived scaling relations and line-of-sight velocity templates using both APOGEE and {\it Gaia} spectroscopic products combined with photometric $G$-band amplitudes. We provide a means to estimate systemic velocities for the RR~Lyrae subclasses, RRab and RRc. Our ana… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.05279v2-abstract-full').style.display = 'inline'; document.getElementById('2404.05279v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.05279v2-abstract-full" style="display: none;"> We present a new set of tools to derive systemic velocities for single-mode RR~Lyrae stars from visual and near-infrared spectra. We derived scaling relations and line-of-sight velocity templates using both APOGEE and {\it Gaia} spectroscopic products combined with photometric $G$-band amplitudes. We provide a means to estimate systemic velocities for the RR~Lyrae subclasses, RRab and RRc. Our analysis indicates that the scaling relation between the photometric and line-of-sight velocity amplitudes is nonlinear, with a break in a linear relation occurring around 0.4mag in both the $V$-band and $G$-band amplitudes. We did not observe such a break in the relation for the first-overtone pulsators. Using stellar pulsation models, we further confirm and examine the nonlinearity in scaling relation for the RRab subclass. We observed little to no variation with stellar parameters (mass, metallicity, and luminosity) in the scaling relation between the photometric and line-of-sight velocity amplitudes for fundamental-mode pulsators. We observed an offset in the scaling relation between the observations and stellar pulsation models, mainly in the low-amplitude RR~Lyrae regime. This offset disappears when different sets of convective parameters are used. Thus, the Fourier amplitudes obtained from the photometry and line-of-sight velocity measurements can be utilized to constrain convective parameters of stellar pulsation models. The scaling relations and templates for APOGEE and {\it Gaia} data accurately predict systemic velocities compared to literature values. In addition, our tools derived from the {\it Gaia} spectra improve the precision of the derived systemic velocities by approximately 50 percent and provide a better description of the uncertainty distribution in comparison with previous studies. Our newly derived tools will be used for RR~Lyrae variables observed toward the Galactic bulge. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.05279v2-abstract-full').style.display = 'none'; document.getElementById('2404.05279v2-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 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">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/2310.19438">arXiv:2310.19438</a> <span> [<a href="https://arxiv.org/pdf/2310.19438">pdf</a>, <a href="https://arxiv.org/format/2310.19438">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The Galactic Bulge exploration I.: The period-absolute\,magnitude-metallicity relations for RR~Lyrae stars for $G_{\rm BP}$, $V$, $G$, $G_{\rm RP}$, $I$, $J$, $H$, and $K_{\rm s}$ passbands using $Gaia$ DR3 parallaxes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Prudil%2C+Z">Z. Prudil</a>, <a href="/search/astro-ph?searchtype=author&query=Kunder%2C+A">A. Kunder</a>, <a href="/search/astro-ph?searchtype=author&query=Dekany%2C+I">I. Dekany</a>, <a href="/search/astro-ph?searchtype=author&query=Koch-Hansen%2C+A+J">A. J Koch-Hansen</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="2310.19438v1-abstract-short" style="display: inline;"> We present a new set of period-absolute magnitude-metallicity (PMZ) relations for single-mode RR Lyrae stars calibrated for the optical $G_{\rm BP}$, $V$, $G$, $G_{\rm RP}$, near-infrared $I$, $J$, $H$, and $K_{\rm s}$ passbands. We compiled a large dataset (over $100$ objects) of fundamental and first-overtone RR~Lyrae pulsators consisting of mean intensity magnitudes, reddenings, pulsations prop… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.19438v1-abstract-full').style.display = 'inline'; document.getElementById('2310.19438v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.19438v1-abstract-full" style="display: none;"> We present a new set of period-absolute magnitude-metallicity (PMZ) relations for single-mode RR Lyrae stars calibrated for the optical $G_{\rm BP}$, $V$, $G$, $G_{\rm RP}$, near-infrared $I$, $J$, $H$, and $K_{\rm s}$ passbands. We compiled a large dataset (over $100$ objects) of fundamental and first-overtone RR~Lyrae pulsators consisting of mean intensity magnitudes, reddenings, pulsations properties, iron abundances, and parallaxes measured by the \textit{Gaia} astrometric satellite in its third data release. Our newly calibrated PMZ relations encapsulate the most up-to-date ingredients in terms of both data and methodology. They are aimed to be used in conjunction with large photometric surveys targeting the Galactic bulge, including the Optical Gravitational Lensing Experiment (OGLE), the Vista Variables in the V铆a L谩ctea Survey (VVV), and the \textit{Gaia} catalog. In addition, our Bayesian probabilistic approach provides accurate uncertainty estimates of the predicted absolute magnitudes of individual RR Lyrae stars. Our derived PMZ relations provide consistent results when compared to benchmark distances to Globular clusters NGC\,6121 (also known as M4), NGC\,5139 (also known as omega Cen), and Large and Small Magellanic Clouds, which are stellar systems rich in RR~Lyrae stars. Lastly, our $K_{\rm s}$-band PMZ relations match well with the previously published PMZ relations based on Gaia data and accurately predict the distance toward the prototype of this class of variables, the eponymic RR~Lyr itself. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.19438v1-abstract-full').style.display = 'none'; document.getElementById('2310.19438v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted 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/2205.14471">arXiv:2205.14471</a> <span> [<a href="https://arxiv.org/pdf/2205.14471">pdf</a>, <a href="https://arxiv.org/format/2205.14471">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Photometric [Fe/H] of RRab stars in the $G$ and $K_s$ bands by deep learning </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Grebel%2C+E+K">Eva K. Grebel</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2205.14471v1-abstract-short" style="display: inline;"> RR Lyrae stars are useful chemical tracers thanks to the empirical relationship between their heavy-element abundance and the shape of their light curves. However, the consistent and accurate calibration of this relation across multiple photometric wavebands has been lacking. We have devised a new method for the metallicity estimation of fundamental-mode RR Lyrae stars in the Gaia optical $G$ and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.14471v1-abstract-full').style.display = 'inline'; document.getElementById('2205.14471v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.14471v1-abstract-full" style="display: none;"> RR Lyrae stars are useful chemical tracers thanks to the empirical relationship between their heavy-element abundance and the shape of their light curves. However, the consistent and accurate calibration of this relation across multiple photometric wavebands has been lacking. We have devised a new method for the metallicity estimation of fundamental-mode RR Lyrae stars in the Gaia optical $G$ and near-infrared VISTA $K_s$ wavebands by deep learning. First, an existing metallicity prediction method is applied to large photometric data sets, which are then used to train long short-term memory recurrent neural networks for the regression of the [Fe/H] to the light curves in other wavebands. This approach allows an unbiased transfer of our accurate, spectroscopically calibrated $I$-band formula to additional bands at the expense of minimal additional noise. We achieve a low mean absolute error of $0.1$ dex and high $R^2$ regression performance of $0.84$ and $0.93$ for the $K_s$ and $G$ bands, respectively, measured by cross-validation. The resulting predictive models are deployed on the Gaia DR2 and VVV inner-bulge RR Lyrae catalogs. We estimate mean metallicities of $-1.35$ dex for the inner bulge and $-1.7$ for the halo, which are significantly less than values obtained by earlier photometric prediction methods. Using our results, we establish a public catalog of photometric metallicities of over 60,000 Galactic RR Lyrae stars, and provide an all-sky map of the resulting RR Lyrae metallicity distribution. The software code used for training and deploying our recurrent neural networks is made publicly available in the open-source domain. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.14471v1-abstract-full').style.display = 'none'; document.getElementById('2205.14471v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in the Astrophysical Journal Supplement Series. Software codes and data are available at: https://github.com/idekany/rrl_feh_nn and https://github.com/idekany/lcfit</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.01137">arXiv:2204.01137</a> <span> [<a href="https://arxiv.org/pdf/2204.01137">pdf</a>, <a href="https://arxiv.org/format/2204.01137">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202243131">10.1051/0004-6361/202243131 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Near infrared and optical emission of WASP-5 b </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kovacs%2C+G">G. Kovacs</a>, <a href="/search/astro-ph?searchtype=author&query=Dekany%2C+I">I. Dekany</a>, <a href="/search/astro-ph?searchtype=author&query=Karamiqucham%2C+B">B. Karamiqucham</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+G">G. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Zhou%2C+G">G. Zhou</a>, <a href="/search/astro-ph?searchtype=author&query=Rabus%2C+M">M. Rabus</a>, <a href="/search/astro-ph?searchtype=author&query=Kovacs%2C+T">T. Kovacs</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="2204.01137v2-abstract-short" style="display: inline;"> CONTEXT: Thermal emission from extrasolar planets makes it possible to study important physical processes in their atmospheres and derive more precise orbital elements. AIMS: By using new near infrared and optical data, we examine how these data constrain the orbital eccentricity and the thermal properties of the planet atmosphere. METHODS: The full light curves acquired by the TESS satellite from… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.01137v2-abstract-full').style.display = 'inline'; document.getElementById('2204.01137v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.01137v2-abstract-full" style="display: none;"> CONTEXT: Thermal emission from extrasolar planets makes it possible to study important physical processes in their atmospheres and derive more precise orbital elements. AIMS: By using new near infrared and optical data, we examine how these data constrain the orbital eccentricity and the thermal properties of the planet atmosphere. METHODS: The full light curves acquired by the TESS satellite from two sectors are used to put upper limit on the amplitude of the planet's phase variation and estimate the occultation depth. Two, already published and one, yet unpublished followup observations in the 2MASS K (Ks) band are employed to derive a more precise occultation light curve in this near infrared waveband. RESULTS: The merged occultation light curve in the Ks band comprises 4515 data points. The data confirm the results of the earlier eccentricity estimates, suggesting circular orbit: e=0.005+/-0.015. The high value of the flux depression of (2.70+/-0.14) ppt in the Ks band excludes simple black body emission at the 10 sigma level and disagrees also with current atmospheric models at the (4-7) sigma level. From the analysis of the TESS data, in the visual band we found tentative evidence for a near noise level detection of the secondary eclipse, and placed constraints on the associated amplitude of the planet's phase variation. A formal box fit yields an occultation depth of (0.157+/-0.056) ppt. This implies a relatively high geometric albedo of Ag=0.43+/-0.15 for fully efficient atmospheric circulation and Ag=0.29+/-0.15 for no circulation at all. No preference can be seen either for the oxygen-enhanced, or for the carbon-enhanced atmosphere models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.01137v2-abstract-full').style.display = 'none'; document.getElementById('2204.01137v2-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 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">After the 2nd referee report. Wrong citation of e*cos(w) by Baskin et al. (2013) has been corrected. Appendix B is supplied by another figure</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 664, A47 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.05983">arXiv:2107.05983</a> <span> [<a href="https://arxiv.org/pdf/2107.05983">pdf</a>, <a href="https://arxiv.org/format/2107.05983">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac106f">10.3847/1538-4357/ac106f <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Metallicity estimation of RR Lyrae stars from their I-band light curves </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Grebel%2C+E+K">Eva K. Grebel</a>, <a href="/search/astro-ph?searchtype=author&query=Pojma%C5%84ski%2C+G">Grzegorz Pojma艅ski</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2107.05983v1-abstract-short" style="display: inline;"> We have revisited the problem of metallicity prediction of RR Lyrae stars from their near-infrared light curves in the Cousins I waveband. Our study is based on high-quality time-series photometry and state-of-the-art high-resolution spectroscopic abundance measurements of 80 fundamental-mode (RRab) and 24 first-overtone (RRc) stars, spanning $\sim$[$-2.7$,$+0.18$] dex and $\sim$[$-3$,$-0.5$] dex… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.05983v1-abstract-full').style.display = 'inline'; document.getElementById('2107.05983v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.05983v1-abstract-full" style="display: none;"> We have revisited the problem of metallicity prediction of RR Lyrae stars from their near-infrared light curves in the Cousins I waveband. Our study is based on high-quality time-series photometry and state-of-the-art high-resolution spectroscopic abundance measurements of 80 fundamental-mode (RRab) and 24 first-overtone (RRc) stars, spanning $\sim$[$-2.7$,$+0.18$] dex and $\sim$[$-3$,$-0.5$] dex ranges, respectively. Employing machine-learning methods, we investigated various light-curve representations and regression models to identify their optimal form for our objective. Accurate new empirical relations between the [Fe/H] iron abundance and the light-curve parameters have been obtained using Bayesian regression for both RRab and RRc stars with mean absolute prediction errors of 0.16 and 0.18 dex, respectively. We found that earlier $I$-band [Fe/H] estimates had a systematic positive bias of up to $\sim 0.4$ dex in the metal-poor regime. Our new predictive models were deployed on large ensembles of RR Lyrae stars to obtain photometric metallicity distribution functions (MDFs) for various old stellar populations in and around the Milky Way. We find that the mode of the old bulge component's MDF is approximately $-1.4$ dex, in remarkable agreement with the latest spectroscopic result. Furthermore, we derive MDF modes of $-1.83$, $-2.13$, and $-1.77$ dex for the Large and Small Magellanic Clouds, and the Sagittarius dwarf galaxy, respectively. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.05983v1-abstract-full').style.display = 'none'; document.getElementById('2107.05983v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in The Astrophysical Journal. Data and codes are available at https://github.com/idekany/ifeh</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2006.09883">arXiv:2006.09883</a> <span> [<a href="https://arxiv.org/pdf/2006.09883">pdf</a>, <a href="https://arxiv.org/format/2006.09883">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ab9d87">10.3847/1538-4357/ab9d87 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Near-Infrared Search for Fundamental-mode RR Lyrae Stars Toward the Inner Bulge by Deep Learning </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Grebel%2C+E+K">Eva K. Grebel</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="2006.09883v1-abstract-short" style="display: inline;"> Aiming to extend the census of RR Lyrae stars to highly reddened low-latitude regions of the central Milky Way, we performed a deep near-IR variability search using data from the VISTA Variables in the V铆a L谩ctea (VVV) survey of the bulge, analyzing the photometric time series of over a hundred million point sources. In order to separate fundamental-mode RR Lyrae (RRab) stars from other periodical… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.09883v1-abstract-full').style.display = 'inline'; document.getElementById('2006.09883v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2006.09883v1-abstract-full" style="display: none;"> Aiming to extend the census of RR Lyrae stars to highly reddened low-latitude regions of the central Milky Way, we performed a deep near-IR variability search using data from the VISTA Variables in the V铆a L谩ctea (VVV) survey of the bulge, analyzing the photometric time series of over a hundred million point sources. In order to separate fundamental-mode RR Lyrae (RRab) stars from other periodically variable sources, we trained a deep bidirectional long short-term memory recurrent neural network (RNN) classifier using VVV survey data and catalogs of RRab stars discovered and classified by optical surveys. Our classifier attained a ~99% precision and recall for light curves with signal-to-noise ratio above 60, and is comparable to the best-performing classifiers trained on accurate optical data. Using our RNN classifier, we identified over 4300 hitherto unknown bona fide RRab stars toward the inner bulge. We provide their photometric catalog and VVV J,H,Ks photometric time-series. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.09883v1-abstract-full').style.display = 'none'; document.getElementById('2006.09883v1-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 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in The Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2001.08272">arXiv:2001.08272</a> <span> [<a href="https://arxiv.org/pdf/2001.08272">pdf</a>, <a href="https://arxiv.org/format/2001.08272">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201936704">10.1051/0004-6361/201936704 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Humps and bumps: The effects of shocks on the optical light curves of fundamental-mode RR Lyrae stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Prudil%2C+Z">Z. Prudil</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=Smolec%2C+R">R. Smolec</a>, <a href="/search/astro-ph?searchtype=author&query=Catelan%2C+M">M. Catelan</a>, <a href="/search/astro-ph?searchtype=author&query=Grebel%2C+E+K">E. K. Grebel</a>, <a href="/search/astro-ph?searchtype=author&query=Kunder%2C+A">A. Kunder</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2001.08272v1-abstract-short" style="display: inline;"> We present the most extended and homogeneous study carried out so far of the main and early shocks in 1485 RR~Lyrae stars in the Galactic bulge observed by the Optical Gravitational Lensing Experiment (OGLE). We selected non-modulated fundamental-mode RR~Lyrae stars with good-quality photometry. Using a self-developed method, we determined the centers and strengths of main and early shock features… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.08272v1-abstract-full').style.display = 'inline'; document.getElementById('2001.08272v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2001.08272v1-abstract-full" style="display: none;"> We present the most extended and homogeneous study carried out so far of the main and early shocks in 1485 RR~Lyrae stars in the Galactic bulge observed by the Optical Gravitational Lensing Experiment (OGLE). We selected non-modulated fundamental-mode RR~Lyrae stars with good-quality photometry. Using a self-developed method, we determined the centers and strengths of main and early shock features in the phased light curves. We found that the position of both humps and bumps are highly correlated with the pulsation properties of the studied variables. Pulsators with a pronounced main shock are concentrated in the low-amplitude regime of the period-amplitude diagram, while stars with a strong early shock have average and above-average pulsation amplitudes. A connection between the main and early shocks and the Fourier coefficients is also observed. In the color-magnitude diagram (CMD), we see a separation between stars with strong and weak shocks. Variables with a pronounced main shock cluster close to the fundamental red edge of the instability strip (IS), while stars with a strong early shock tend to clump in the center and near the fundamental blue edge of the IS. The appearance of shocks and their properties seem independent of the direction of evolution estimated from the period change rate of the studied stars. In addition, the differences in the period change rate between the two main Oosterhoff groups found in the Galactic bulge suggest that stars of Oosterhoff type I are located close to the zero-age horizontal branch while Oosterhoff type II variables are on their way toward the fundamental red edge of the instability strip, thus having already left the zero-age horizontal branch. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.08272v1-abstract-full').style.display = 'none'; document.getElementById('2001.08272v1-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 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 10 figures, Accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 635, A66 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2001.05536">arXiv:2001.05536</a> <span> [<a href="https://arxiv.org/pdf/2001.05536">pdf</a>, <a href="https://arxiv.org/format/2001.05536">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/staa155">10.1093/mnras/staa155 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> VVV-WIT-01: highly obscured classical nova or protostellar collision? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+P+W">P. W. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Kamble%2C+A">A. Kamble</a>, <a href="/search/astro-ph?searchtype=author&query=Kaplan%2C+D+L">D. L. Kaplan</a>, <a href="/search/astro-ph?searchtype=author&query=Cross%2C+N">N. Cross</a>, <a href="/search/astro-ph?searchtype=author&query=Dekany%2C+I">I. Dekany</a>, <a href="/search/astro-ph?searchtype=author&query=Ivanov%2C+V+D">V. D. Ivanov</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtev%2C+R">R. Kurtev</a>, <a href="/search/astro-ph?searchtype=author&query=Saito%2C+R+K">R. K. Saito</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+L+C">L. C. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Catelan%2C+M">M. Catelan</a>, <a href="/search/astro-ph?searchtype=author&query=Masetti%2C+N">N. Masetti</a>, <a href="/search/astro-ph?searchtype=author&query=Toledo%2C+I">I. Toledo</a>, <a href="/search/astro-ph?searchtype=author&query=Hempel%2C+M">M. Hempel</a>, <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+M+A">M. A. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Pe%C3%B1a%2C+C+C">C. Contreras Pe帽a</a>, <a href="/search/astro-ph?searchtype=author&query=Forbrich%2C+J">J. Forbrich</a>, <a href="/search/astro-ph?searchtype=author&query=Krause%2C+M">M. Krause</a>, <a href="/search/astro-ph?searchtype=author&query=Dale%2C+J">J. Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Borissova%2C+J">J. Borissova</a>, <a href="/search/astro-ph?searchtype=author&query=Emerson%2C+J">J. Emerson</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2001.05536v1-abstract-short" style="display: inline;"> A search of the first Data Release of the VISTA Variables in the Via Lactea (VVV) Survey discovered the exceptionally red transient VVV-WIT-01 ($H-K_s=5.2$). It peaked before March 2010, then faded by $\sim$9.5 mag over the following two years. The 1.6--22 $渭$m spectral energy distribution in March 2010 was well fit by a highly obscured black body with $T \sim 1000$ K and $A_{K_s} \sim 6.6$ mag. T… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.05536v1-abstract-full').style.display = 'inline'; document.getElementById('2001.05536v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2001.05536v1-abstract-full" style="display: none;"> A search of the first Data Release of the VISTA Variables in the Via Lactea (VVV) Survey discovered the exceptionally red transient VVV-WIT-01 ($H-K_s=5.2$). It peaked before March 2010, then faded by $\sim$9.5 mag over the following two years. The 1.6--22 $渭$m spectral energy distribution in March 2010 was well fit by a highly obscured black body with $T \sim 1000$ K and $A_{K_s} \sim 6.6$ mag. The source is projected against the Infrared Dark Cloud (IRDC) SDC G331.062$-$0.294. The chance projection probability is small for any single event ($p \approx 0.01$ to 0.02) which suggests a physical association, e.g. a collision between low mass protostars. However, black body emission at $T \sim 1000$ K is common in classical novae (especially CO novae) at the infrared peak in the light curve, due to condensation of dust $\sim$30--60 days after the explosion. Radio follow up with the Australia Telescope Compact Array (ATCA) detected a fading continuum source with properties consistent with a classical nova but probably inconsistent with colliding protostars. Considering all VVV transients that could have been projected against a catalogued IRDC raises the probability of a chance association to $p=0.13$ to 0.24. After weighing several options, it appears likely that VVV-WIT-01 was a classical nova event located behind an IRDC. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.05536v1-abstract-full').style.display = 'none'; document.getElementById('2001.05536v1-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 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 7 figures. Accepted by MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2001.02486">arXiv:2001.02486</a> <span> [<a href="https://arxiv.org/pdf/2001.02486">pdf</a>, <a href="https://arxiv.org/format/2001.02486">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/staa046">10.1093/mnras/staa046 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Evidence for Galactic disc RR~Lyrae stars in the Solar neighbourhood </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Prudil%2C+Z">Z. Prudil</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=Grebel%2C+E+K">E. K. Grebel</a>, <a href="/search/astro-ph?searchtype=author&query=Kunder%2C+A">A. Kunder</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2001.02486v3-abstract-short" style="display: inline;"> We present a kinematical study of 314 RR~Lyrae stars in the solar neighbourhood using the publicly available photometric, spectroscopic, and {\it Gaia} DR2 astrometric data to explore their distribution in the Milky Way. We report an overdensity of 22 RR~Lyrae stars in the solar neighbourhood at a pericenter distance of between 5--9\,kpc from the Galactic center. Their orbital parameters and their… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.02486v3-abstract-full').style.display = 'inline'; document.getElementById('2001.02486v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2001.02486v3-abstract-full" style="display: none;"> We present a kinematical study of 314 RR~Lyrae stars in the solar neighbourhood using the publicly available photometric, spectroscopic, and {\it Gaia} DR2 astrometric data to explore their distribution in the Milky Way. We report an overdensity of 22 RR~Lyrae stars in the solar neighbourhood at a pericenter distance of between 5--9\,kpc from the Galactic center. Their orbital parameters and their chemistry indicate that these 22 variables share the kinematics and the [Fe/H] values of the Galactic disc, with an average metallicity and tangential velocity of [Fe/H]=$-0.60$\,dex and $v_胃 = 241$\,km\,s$^{-1}$, respectively. From the distribution of the Galactocentric spherical velocity components, we find that these 22 disc-like RR~Lyrae variables are not consistent with the {\it Gaia} Sausage ({\it Gaia}-Enceladus), unlike almost half of the local RR~Lyrae stars. Chemical information from the literature shows that the majority of the selected pericenter peak RR~Lyrae variables are $伪$-poor, a property shared by typically much younger stars in the thin disc. Using the available photometry we rule out a possible misclassification with the known classical and anomalous Cepheids. The similar kinematic, chemical, and pulsation properties of these disc RR~Lyrae stars suggest they share a common origin. In contrast, we find the RR~Lyrae stars associated with the {\it Gaia}-Enceladus based on their kinematics and chemical composition show a considerable metallicity spread in the old population ($\sim$~1\,dex). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.02486v3-abstract-full').style.display = 'none'; document.getElementById('2001.02486v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 9 figures, Accepted for publication in MNRAS, final version</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1908.08290">arXiv:1908.08290</a> <span> [<a href="https://arxiv.org/pdf/1908.08290">pdf</a>, <a href="https://arxiv.org/format/1908.08290">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ab3b60">10.3847/1538-4357/ab3b60 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Into the Darkness: Classical and Type II Cepheids in the Zona Galactica Incognita </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Hajdu%2C+G">Gergely Hajdu</a>, <a href="/search/astro-ph?searchtype=author&query=Grebel%2C+E+K">Eva K. Grebel</a>, <a href="/search/astro-ph?searchtype=author&query=Catelan%2C+M">M谩rcio Catelan</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="1908.08290v1-abstract-short" style="display: inline;"> The far side of the Milky Way's disk is one of the most concealed parts of the known Universe due to extremely high interstellar extinction and point source density toward low Galactic latitudes. Large time-domain photometric surveys operating in the near-infrared hold great potential for the exploration of these vast uncharted areas of our Galaxy. We conducted a census of distant classical and ty… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.08290v1-abstract-full').style.display = 'inline'; document.getElementById('1908.08290v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1908.08290v1-abstract-full" style="display: none;"> The far side of the Milky Way's disk is one of the most concealed parts of the known Universe due to extremely high interstellar extinction and point source density toward low Galactic latitudes. Large time-domain photometric surveys operating in the near-infrared hold great potential for the exploration of these vast uncharted areas of our Galaxy. We conducted a census of distant classical and type II Cepheids along the southern Galactic mid-plane using near-infrared photometry from the VISTA Variables in the V铆a L谩ctea survey. We performed a machine-learned classification of the Cepheids based on their infrared light curves using a convolutional neural network. We have discovered 640 distant classical Cepheids with up to ~40 magnitudes of visual extinction, and over 500 type II Cepheids, most of them located in the inner bulge. Intrinsic color indices of individual Cepheids were predicted from sparse photometric data using a neural network, allowing their use as accurate reddening tracers. They revealed a steep, spatially varying near-infrared extinction curve toward the inner bulge. Type II Cepheids in the Galactic bulge were also employed to measure robust mean selective-to-absolute extinction ratios. They trace a centrally concentrated spatial distribution of the old bulge population with a slight elongation, consistent with earlier results from RR Lyrae stars. Likewise, the classical Cepheids were utilized to trace the Galactic warp and various substructures of the Galactic disk, and to uncover significant vertical and radial age gradients of the thin disk population at the far side of the Milky Way. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.08290v1-abstract-full').style.display = 'none'; document.getElementById('1908.08290v1-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 August, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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 by The Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1908.06160">arXiv:1908.06160</a> <span> [<a href="https://arxiv.org/pdf/1908.06160">pdf</a>, <a href="https://arxiv.org/format/1908.06160">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1007/s10686-020-09661-0">10.1007/s10686-020-09661-0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> On the optimal calibration of VVV photometry </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hajdu%2C+G">Gergely Hajdu</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=Catelan%2C+M">M谩rcio Catelan</a>, <a href="/search/astro-ph?searchtype=author&query=Grebel%2C+E+K">Eva K. Grebel</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="1908.06160v2-abstract-short" style="display: inline;"> Prompted by some inconsistencies in the photometry of the VISTA Variables in the V铆a L谩ctea (VVV) survey, we conduct a revision of the standard calibration procedure of VISTA data in the $J$, $H$, and $K_S$ passbands. Two independent sources of bias in the photometric zero-points are identified: First, high sky backgrounds severely affect the $H$-band measurements, but this can mostly be minimized… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.06160v2-abstract-full').style.display = 'inline'; document.getElementById('1908.06160v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1908.06160v2-abstract-full" style="display: none;"> Prompted by some inconsistencies in the photometry of the VISTA Variables in the V铆a L谩ctea (VVV) survey, we conduct a revision of the standard calibration procedure of VISTA data in the $J$, $H$, and $K_S$ passbands. Two independent sources of bias in the photometric zero-points are identified: First, high sky backgrounds severely affect the $H$-band measurements, but this can mostly be minimized by strict data vetting. Secondly, during the zero-point calibration, stars serving as standards are taken from the 2MASS catalog, which can suffer from high degrees of blending in regions of high stellar density, affecting both the absolute photometric calibration, as well as the scatter of repeated observations. The former affects studies that rely on an absolute magnitude scale, while the latter can also affect the shapes and amount of scatter in the VVV light curves, thus potentially hampering their proper classification. We show that these errors can be effectively eliminated by relatively simple modifications of the standard calibration procedure, and demonstrate the effect of the recalibration on the VVV survey's data quality. We give recommendations for future improvements of the pipeline calibration of VISTA photometry, while also providing preliminary corrections to the VVV $JHK_\mathrm{S}$ observations as a temporary measure. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.06160v2-abstract-full').style.display = 'none'; document.getElementById('1908.06160v2-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 May, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 August, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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 Experimental Astronomy; Table 1 is available from the first author upon request</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1905.11870">arXiv:1905.11870</a> <span> [<a href="https://arxiv.org/pdf/1905.11870">pdf</a>, <a href="https://arxiv.org/format/1905.11870">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stz1484">10.1093/mnras/stz1484 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> On the Oosterhoff dichotomy in the Galactic bulge: II. kinematical distribution </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Prudil%2C+Z">Z. Prudil</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=Grebel%2C+E+K">E. K. Grebel</a>, <a href="/search/astro-ph?searchtype=author&query=Catelan%2C+M">M. Catelan</a>, <a href="/search/astro-ph?searchtype=author&query=Skarka%2C+M">M. Skarka</a>, <a href="/search/astro-ph?searchtype=author&query=Smolec%2C+R">R. Smolec</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="1905.11870v1-abstract-short" style="display: inline;"> We present a kinematical study of RR~Lyrae stars associated with two Oosterhoff groups in the Galactic bulge. We used data published in the first paper of the series, plus proper motions from the {\it Gaia} Data Release 2, and radial velocities from the literature. A 6D kinematical and spatial solution was obtained for 429 RR~Lyrae stars. We use a model of the Galactic gravitational potential to i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.11870v1-abstract-full').style.display = 'inline'; document.getElementById('1905.11870v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1905.11870v1-abstract-full" style="display: none;"> We present a kinematical study of RR~Lyrae stars associated with two Oosterhoff groups in the Galactic bulge. We used data published in the first paper of the series, plus proper motions from the {\it Gaia} Data Release 2, and radial velocities from the literature. A 6D kinematical and spatial solution was obtained for 429 RR~Lyrae stars. We use a model of the Galactic gravitational potential to infer stellar orbits. We did not find a difference between the Oosterhoff groups in the individual components of the space velocity. We report that \textit{foreground} and \textit{background} stars with respect to the Galactic bulge stand out in the mean $V$ velocity component, which we interpret as a sign of the Galactic rotation. The movement of the studied stars in the central region of the Galactic bulge is consistent with random motions expected for a classical bulge component. From the orbital integration, we estimate that 8\,\% of the RR~Lyrae stars are halo interlopers currently located in the Galactic bulge. The majority of the stars' orbits are within a 3\,kpc radius from the Galactic bulge. The fraction of Oosterhoff\,II stars increases with increasing Galactic latitude, as well as towards longer orbital periods. We found several RR~Lyrae stars with high space velocities, one of which has an extremely long orbital period of $\sim$1\,Gyr. We conclude that based on their kinematics, the vast majority of the stars in our sample do not seem to contribute to the boxy/peanut component of the Galactic bulge. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.11870v1-abstract-full').style.display = 'none'; document.getElementById('1905.11870v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 May, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">11 pages, 8 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/1901.09726">arXiv:1901.09726</a> <span> [<a href="https://arxiv.org/pdf/1901.09726">pdf</a>, <a href="https://arxiv.org/format/1901.09726">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stz311">10.1093/mnras/stz311 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> On the Oosterhoff dichotomy in the Galactic bulge: I. spatial distribution </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Prudil%2C+Z">Z. Prudil</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=Catelan%2C+M">M. Catelan</a>, <a href="/search/astro-ph?searchtype=author&query=Smolec%2C+R">R. Smolec</a>, <a href="/search/astro-ph?searchtype=author&query=Grebel%2C+E+K">E. K. Grebel</a>, <a href="/search/astro-ph?searchtype=author&query=Skarka%2C+M">M. Skarka</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1901.09726v1-abstract-short" style="display: inline;"> We present a study of the Oosterhoff (Oo) dichotomy in the Galactic bulge using 8\,141 fundamental mode RR~Lyrae stars. We used public photometric data from the Optical Gravitational Lensing Experiment (OGLE) and the Vista Variables in the V铆a L谩ctea survey (VVV). We carefully selected fundamental mode stars without modulation and without association with any globular cluster located toward the Ga… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.09726v1-abstract-full').style.display = 'inline'; document.getElementById('1901.09726v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1901.09726v1-abstract-full" style="display: none;"> We present a study of the Oosterhoff (Oo) dichotomy in the Galactic bulge using 8\,141 fundamental mode RR~Lyrae stars. We used public photometric data from the Optical Gravitational Lensing Experiment (OGLE) and the Vista Variables in the V铆a L谩ctea survey (VVV). We carefully selected fundamental mode stars without modulation and without association with any globular cluster located toward the Galactic bulge. Subsequently, we identified and separated the Oosterhoff groups I and II on the basis of their period-amplitude distribution and using a relation fitted to the Oosterhoff I locus. Both Oosterhoff groups were then compared to observations of two bulge globular clusters and with models of stellar pulsation and evolution. We found that some of the variables classified as Oo\,II belong to a third Oo group. The Oosterhoff II variables are more metal-poor on average, more massive, and cooler than their Oosterhoff I counterparts. The analysis of their spatial distribution shows a systematic difference between \textit{foreground}, central and \textit{background} regions in the occurrence of the Oosterhoff II group. The difference between the Oo\,I and II groups is also seen in their distance distributions with respect to the Galactic bar, but neither group is associated with the bar. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.09726v1-abstract-full').style.display = 'none'; document.getElementById('1901.09726v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 January, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 12 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/1809.06087">arXiv:1809.06087</a> <span> [<a href="https://arxiv.org/pdf/1809.06087">pdf</a>, <a href="https://arxiv.org/format/1809.06087">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/sty1885">10.1093/mnras/sty1885 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Photometric study of the SMCNOD using variable stars from the OGLE-IV survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Prudil%2C+Z">Z. Prudil</a>, <a href="/search/astro-ph?searchtype=author&query=Grebel%2C+E+K">E. K. Grebel</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=Smolec%2C+R">R. Smolec</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1809.06087v1-abstract-short" style="display: inline;"> We present a study of a recently discovered stellar overdensity near the northern edge of the Small Magellanic Cloud (SMCNOD). We exploited variable stars from the fourth release of the Optical Gravitational Lensing Experiment (OGLE). We used mainly pulsating variable stars and investigated their potential association with the SMCNOD using their spatial distribution and distances. We found four ra… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1809.06087v1-abstract-full').style.display = 'inline'; document.getElementById('1809.06087v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1809.06087v1-abstract-full" style="display: none;"> We present a study of a recently discovered stellar overdensity near the northern edge of the Small Magellanic Cloud (SMCNOD). We exploited variable stars from the fourth release of the Optical Gravitational Lensing Experiment (OGLE). We used mainly pulsating variable stars and investigated their potential association with the SMCNOD using their spatial distribution and distances. We found four rather spatially concentrated anomalous Cepheids and eight evenly dispersed RR~Lyrae stars to be most likely members of this overdensity. The anomalous Cepheids inside the SMCNOD trace possible intermediate-age population with ages ranging between $2-4.5$ Gyr. The age distribution of anomalous Cepheids seems to be in a good agreement with the age distribution of anomalous Cepheids in the SMC. Using empirical relations for RR~Lyrae stars we determined the median metallicity for a possible old population in the SMCNOD to be $\rm [Fe/H]_{\rm SMCNOD}=-1.71\pm0.21$ dex, which is in agreement with median metallicity of the old SMC population. The density profile for anomalous Cepheids shows a small anomaly at the position of the SMCNOD, on the other hand, RR~Lyrae variables show no such deviation. The probability of finding the observed number of variable stars at the location of the SMCNOD by chance is very low for anomalous Cepheids (0.7 %) but high for RR~Lyrae stars (13.0 %). Based on its variable stars content, we thus confirm the presence of a modest overdensity in intermediate-age stars in the SMCNOD and conclude that it probably has its origin in the SMC rather than to be the remnant of an accreted dwarf galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1809.06087v1-abstract-full').style.display = 'none'; document.getElementById('1809.06087v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 September, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 14 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/1805.04119">arXiv:1805.04119</a> <span> [<a href="https://arxiv.org/pdf/1805.04119">pdf</a>, <a href="https://arxiv.org/ps/1805.04119">ps</a>, <a href="https://arxiv.org/format/1805.04119">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/10.1007/s10509-018-3346-6">10.1007/s10509-018-3346-6 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Establishing the Galactic Centre Distance Using VVV Bulge RR Lyrae Variables </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Majaess%2C+D">D. Majaess</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=Hajdu%2C+G">G. Hajdu</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Turner%2C+D+G">D. G. Turner</a>, <a href="/search/astro-ph?searchtype=author&query=Gieren%2C+W">W. Gieren</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1805.04119v1-abstract-short" style="display: inline;"> This study's objective was to exploit infrared VVV (VISTA Variables in the Via Lactea) photometry for high latitude RRab stars to establish an accurate Galactic Centre distance. RRab candidates were discovered and reaffirmed ($n=4194$) by matching $K_s$ photometry with templates via $蠂^2$ minimization, and contaminants were reduced by ensuring targets adhered to a strict period-amplitude ($螖K_s$)… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.04119v1-abstract-full').style.display = 'inline'; document.getElementById('1805.04119v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1805.04119v1-abstract-full" style="display: none;"> This study's objective was to exploit infrared VVV (VISTA Variables in the Via Lactea) photometry for high latitude RRab stars to establish an accurate Galactic Centre distance. RRab candidates were discovered and reaffirmed ($n=4194$) by matching $K_s$ photometry with templates via $蠂^2$ minimization, and contaminants were reduced by ensuring targets adhered to a strict period-amplitude ($螖K_s$) trend and passed the Elorietta et al. classifier. The distance to the Galactic Centre was determined from a high latitude Bulge subsample ($|b|>4^{o}$, $R_{GC}=8.30 \pm 0.36$ kpc, random uncertainty is relatively negligible), and importantly, the comparatively low color-excess and uncrowded location mitigated uncertainties tied to the extinction law, the magnitude-limited nature of the analysis, and photometric contamination. Circumventing those problems resulted in a key uncertainty being the $M_{K_s}$ relation, which was derived using LMC RRab stars ($M_{K_s}=-(2.66\pm0.06) \log{P}-(1.03\pm0.06)$, $(J-K_s)_0=(0.31\pm0.04) \log{P} + (0.35\pm0.02)$, assuming $渭_{0,LMC}=18.43$). The Galactic Centre distance was not corrected for the cone-effect. Lastly, a new distance indicator emerged as brighter overdensities in the period-magnitude-amplitude diagrams analyzed, which arise from blended RRab and red clump stars. Blending may thrust faint extragalactic variables into the range of detectability. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.04119v1-abstract-full').style.display = 'none'; document.getElementById('1805.04119v1-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 May, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">To appear in Ap&SS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1804.01457">arXiv:1804.01457</a> <span> [<a href="https://arxiv.org/pdf/1804.01457">pdf</a>, <a href="https://arxiv.org/format/1804.01457">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/aab4fa">10.3847/1538-4357/aab4fa <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Near-infrared RR Lyrae census along the southern Galactic plane: the Milky Way's stellar fossil brought to light </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Hajdu%2C+G">Gergely Hajdu</a>, <a href="/search/astro-ph?searchtype=author&query=Grebel%2C+E+K">Eva K. Grebel</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=Elorrieta%2C+F">Felipe Elorrieta</a>, <a href="/search/astro-ph?searchtype=author&query=Eyheramendy%2C+S">Susana Eyheramendy</a>, <a href="/search/astro-ph?searchtype=author&query=Majaess%2C+D">Daniel Majaess</a>, <a href="/search/astro-ph?searchtype=author&query=Jord%C3%A1n%2C+A">Andr茅s Jord谩n</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="1804.01457v1-abstract-short" style="display: inline;"> RR Lyrae stars (RRLs) are tracers of the Milky Way's fossil record, holding valuable information on its formation and early evolution. Owing to the high interstellar extinction endemic to the Galactic plane, distant RRLs lying at low Galactic latitudes have been elusive. We attained a census of 1892 high-confidence RRLs by exploiting the near-infrared photometric database of the VVV survey's disk… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.01457v1-abstract-full').style.display = 'inline'; document.getElementById('1804.01457v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1804.01457v1-abstract-full" style="display: none;"> RR Lyrae stars (RRLs) are tracers of the Milky Way's fossil record, holding valuable information on its formation and early evolution. Owing to the high interstellar extinction endemic to the Galactic plane, distant RRLs lying at low Galactic latitudes have been elusive. We attained a census of 1892 high-confidence RRLs by exploiting the near-infrared photometric database of the VVV survey's disk footprint spanning $\sim$70$^\circ$ of Galactic longitude, using a machine-learned classifier. Novel data-driven methods were employed to accurately characterize their spatial distribution using sparsely sampled multi-band photometry. The RRL metallicity distribution function (MDF) was derived from their $K_s$-band light curve parameters using machine-learning methods. The MDF shows remarkable structural similarities to both the spectroscopic MDF of red clump giants and the MDF of bulge RRLs. We model the MDF with a multi-component density distribution and find that the number density of stars associated with the different model components systematically changes with both the Galactocentric radius and vertical distance from the Galactic plane, equivalent to weak metallicity gradients. Based on the consistency with results from the ARGOS survey, three MDF modes are attributed to the old disk populations, while the most metal-poor RRLs are probably halo interlopers. We propose that the dominant [Fe/H] component with a mean of $-1$ dex might correspond to the outskirts of an ancient Galactic spheroid or classical bulge component residing in the central Milky Way. The physical origins of the RRLs in this study need to be verified by kinematical information. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.01457v1-abstract-full').style.display = 'none'; document.getElementById('1804.01457v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 April, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">ApJ, in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1804.01456">arXiv:1804.01456</a> <span> [<a href="https://arxiv.org/pdf/1804.01456">pdf</a>, <a href="https://arxiv.org/format/1804.01456">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/aab4fd">10.3847/1538-4357/aab4fd <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Data-driven Study of RR Lyrae Near-IR Light Curves: Principal Component Analysis, Robust Fits, and Metallicity Estimates </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hajdu%2C+G">Gergely Hajdu</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=Catelan%2C+M">M谩rcio Catelan</a>, <a href="/search/astro-ph?searchtype=author&query=Grebel%2C+E+K">Eva K. Grebel</a>, <a href="/search/astro-ph?searchtype=author&query=Jurcsik%2C+J">Johanna Jurcsik</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="1804.01456v1-abstract-short" style="display: inline;"> RR~Lyrae variables are widely used tracers of Galactic halo structure and kinematics, but they can also serve to constrain the distribution of the old stellar population in the Galactic bulge. With the aim of improving their near-infrared photometric characterization, we investigate their near-infrared light curves, as well as the empirical relationships between their light curve and metallicities… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.01456v1-abstract-full').style.display = 'inline'; document.getElementById('1804.01456v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1804.01456v1-abstract-full" style="display: none;"> RR~Lyrae variables are widely used tracers of Galactic halo structure and kinematics, but they can also serve to constrain the distribution of the old stellar population in the Galactic bulge. With the aim of improving their near-infrared photometric characterization, we investigate their near-infrared light curves, as well as the empirical relationships between their light curve and metallicities using machine learning methods. We introduce a new, robust method for the estimation of the light-curve shapes, and hence the average magnitudes of RR~Lyrae variables in the $K_\mathrm{S}$ band, by utilizing the first few principal components (PCs) as basis vectors, obtained from the PC analysis of a training set of light curves. Furthermore, we use the amplitudes of these PCs to predict the light-curve shape of each star in the $J$-band, allowing us to precisely determine their average magnitudes (hence colors), even in cases where only one $J$ measurement is available. Finally, we demonstrate that the $K_\mathrm{S}$-band light-curve parameters of RR~Lyrae variables, together with the period, allow the estimation of the metallicity of individual stars with an accuracy of $\sim 0.2 - 0.25$ dex, providing valuable chemical information about old stellar populations bearing RR~Lyrae variables. The methods presented here can be straightforwardly adopted for other classes of variable stars, bands, or for the estimation of other physical quantities. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.01456v1-abstract-full').style.display = 'none'; document.getElementById('1804.01456v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 April, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in the Astrophysical Journal; 21 pages, 14 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1801.03436">arXiv:1801.03436</a> <span> [<a href="https://arxiv.org/pdf/1801.03436">pdf</a>, <a href="https://arxiv.org/ps/1801.03436">ps</a>, <a href="https://arxiv.org/format/1801.03436">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/sty112">10.1093/mnras/sty112 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Blazhko modulation in the infrared </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jurcsik%2C+J">J. Jurcsik</a>, <a href="/search/astro-ph?searchtype=author&query=Hajdu%2C+G">G. Hajdu</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=Nuspl%2C+J">J. Nuspl</a>, <a href="/search/astro-ph?searchtype=author&query=Catelan%2C+M">M. Catelan</a>, <a href="/search/astro-ph?searchtype=author&query=Grebel%2C+E+K">E. K. Grebel</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1801.03436v1-abstract-short" style="display: inline;"> We present first direct evidence of modulation in the $K$-band of Blazhko-type RR Lyrae stars that are identified by their secular modulations in the I-band data of OGLE-IV. A method has been developed to decompose the $K$-band light variation into two parts originating from the temperature and the radius changes using synthetic data of atmosphere-model grids. The amplitudes of the temperature and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.03436v1-abstract-full').style.display = 'inline'; document.getElementById('1801.03436v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1801.03436v1-abstract-full" style="display: none;"> We present first direct evidence of modulation in the $K$-band of Blazhko-type RR Lyrae stars that are identified by their secular modulations in the I-band data of OGLE-IV. A method has been developed to decompose the $K$-band light variation into two parts originating from the temperature and the radius changes using synthetic data of atmosphere-model grids. The amplitudes of the temperature and the radius variations derived from the method for non-Blazhko RRab stars are in very good agreement with the results of the Baade-Wesselink analysis of RRab stars in the M3 globular cluster confirming the applicability and correctness of the method. It has been found that the Blazhko modulation is primarily driven by the change in the temperature variation. The radius variation plays a marginal part, moreover it has an opposite sign as if the Blazhko effect was caused by the radii variations. This result reinforces the previous finding based on the Baade-Wesselink analysis of M3 (NGC 5272) RR Lyrae, that significant modulation of the radius variations can only be detected in radial-velocity measurements, which relies on spectral lines that form in the uppermost atmospheric layers. Our result gives the first insight into the energetics and dynamics of the Blazhko phenomenon, hence it puts strong constraints on its possible physical explanations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.03436v1-abstract-full').style.display = 'none'; document.getElementById('1801.03436v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 January, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 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/1706.03899">arXiv:1706.03899</a> <span> [<a href="https://arxiv.org/pdf/1706.03899">pdf</a>, <a href="https://arxiv.org/format/1706.03899">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/epjconf/201715207005">10.1051/epjconf/201715207005 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Pulsating stars in $蠅$ Centauri: Near-IR properties and period-luminosity relations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Navarrete%2C+C">Camila Navarrete</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=Ramos%2C+R+C">Rodrigo Contreras Ramos</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=Gran%2C+F">Felipe Gran</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=Minniti%2C+D">Dante Minniti</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1706.03899v1-abstract-short" style="display: inline;"> $蠅$ Centauri (NGC~5139) contains many variable stars of different types, including the pulsating type II Cepheids, RR Lyrae and SX Phoenicis stars. We carried out a deep, wide-field, near-infrared (IR) variability survey of $蠅$ Cen, using the VISTA telescope. We assembled an unprecedented homogeneous and complete $J$ and $K_{\rm S}$ near-IR catalog of variable stars in the field of $蠅$ Cen. In thi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1706.03899v1-abstract-full').style.display = 'inline'; document.getElementById('1706.03899v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1706.03899v1-abstract-full" style="display: none;"> $蠅$ Centauri (NGC~5139) contains many variable stars of different types, including the pulsating type II Cepheids, RR Lyrae and SX Phoenicis stars. We carried out a deep, wide-field, near-infrared (IR) variability survey of $蠅$ Cen, using the VISTA telescope. We assembled an unprecedented homogeneous and complete $J$ and $K_{\rm S}$ near-IR catalog of variable stars in the field of $蠅$ Cen. In this paper we compare optical and near-IR light curves of RR Lyrae stars, emphasizing the main differences. Moreover, we discuss the ability of near-IR observations to detect SX Phoenicis stars given the fact that the amplitudes are much smaller in these bands compared to the optical. Finally, we consider the case in which all the pulsating stars in the three different variability types follow a single period-luminosity relation in the near-IR bands. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1706.03899v1-abstract-full').style.display = 'none'; document.getElementById('1706.03899v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 June, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Conference Proceedings. Wide-field variability surveys: a 21st-century perspective. 6 pages, 4 figures, in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1704.03031">arXiv:1704.03031</a> <span> [<a href="https://arxiv.org/pdf/1704.03031">pdf</a>, <a href="https://arxiv.org/format/1704.03031">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/10.1051/0004-6361/201630102">10.1051/0004-6361/201630102 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Near-IR period-luminosity relations for pulsating stars in $蠅$ Centauri (NGC 5139) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Navarrete%2C+C">C. Navarrete</a>, <a href="/search/astro-ph?searchtype=author&query=Catelan%2C+M">M. Catelan</a>, <a href="/search/astro-ph?searchtype=author&query=Ramos%2C+R+C">R. Contreras Ramos</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=Gran%2C+F">F. Gran</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=Minniti%2C+D">D. Minniti</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1704.03031v1-abstract-short" style="display: inline;"> $蠅$ Centauri (NGC 5139) hosts hundreds of pulsating variable stars of different types, thus representing a treasure trove for studies of their corresponding period-luminosity (PL) relations. Our goal in this study is to obtain the PL relations for RR Lyrae, and SX Phoenicis stars in the field of the cluster, based on high-quality, well-sampled light curves in the near-infrared (IR). $蠅… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1704.03031v1-abstract-full').style.display = 'inline'; document.getElementById('1704.03031v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1704.03031v1-abstract-full" style="display: none;"> $蠅$ Centauri (NGC 5139) hosts hundreds of pulsating variable stars of different types, thus representing a treasure trove for studies of their corresponding period-luminosity (PL) relations. Our goal in this study is to obtain the PL relations for RR Lyrae, and SX Phoenicis stars in the field of the cluster, based on high-quality, well-sampled light curves in the near-infrared (IR). $蠅$ Centauri was observed using VIRCAM mounted on VISTA. A total of 42 epochs in $J$ and 100 epochs in $K_{\rm S}$ were obtained, spanning 352 days. Point-spread function photometry was performed using DoPhot and DAOPHOT in the outer and inner regions of the cluster, respectively. Based on the comprehensive catalogue of near-IR light curves thus secured, PL relations were obtained for the different types of pulsators in the cluster, both in the $J$ and $K_{\rm S}$ bands. This includes the first PL relations in the near-IR for fundamental-mode SX Phoenicis stars. The near-IR magnitudes and periods of Type II Cepheids and RR Lyrae stars were used to derive an updated true distance modulus to the cluster, with a resulting value of $(m-M)_0 = 13.708 \pm 0.035 \pm 0.10$ mag, where the error bars correspond to the adopted statistical and systematic errors, respectively. Adding the errors in quadrature, this is equivalent to a heliocentric distance of $5.52\pm 0.27$ kpc. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1704.03031v1-abstract-full').style.display = 'none'; document.getElementById('1704.03031v1-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 April, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 8 figures, accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 604, A120 (2017) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1703.02033">arXiv:1703.02033</a> <span> [<a href="https://arxiv.org/pdf/1703.02033">pdf</a>, <a href="https://arxiv.org/format/1703.02033">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/838/1/L14">10.3847/2041-8213/838/1/L14 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> FSR 1716: A new Milky Way Globular Cluster confirmed using VVV RR Lyrae stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">Dante Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Palma%2C+T">Tali Palma</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%A9k%C3%A1ny%2C+I">Istvan D茅k谩ny</a>, <a href="/search/astro-ph?searchtype=author&query=Hempel%2C+M">Maren Hempel</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">Marina Rejkuba</a>, <a href="/search/astro-ph?searchtype=author&query=Pullen%2C+J">Joyce Pullen</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=Barb%C3%A1%2C+R">Rodolfo 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=Bica%2C+E">Eduardo Bica</a>, <a href="/search/astro-ph?searchtype=author&query=Bonatto%2C+C">Charles Bonatto</a>, <a href="/search/astro-ph?searchtype=author&query=Borissova%2C+J">Jura Borissova</a>, <a href="/search/astro-ph?searchtype=author&query=Catelan%2C+M">Marcio Catelan</a>, <a href="/search/astro-ph?searchtype=author&query=Carballo-Bello%2C+J+A">Julio A. Carballo-Bello</a>, <a href="/search/astro-ph?searchtype=author&query=Chene%2C+A+N">Andre Nicolas Chene</a>, <a href="/search/astro-ph?searchtype=author&query=Clari%C3%A1%2C+J+J">Juan J. Clari谩</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R+E">Roger E. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Contreras-Ramos%2C+R">Rodrigo Contreras-Ramos</a>, <a href="/search/astro-ph?searchtype=author&query=Dias%2C+B">Bruno Dias</a>, <a href="/search/astro-ph?searchtype=author&query=Emerson%2C+J">Jim Emerson</a>, <a href="/search/astro-ph?searchtype=author&query=Froebrich%2C+D">Dirk Froebrich</a>, <a href="/search/astro-ph?searchtype=author&query=Buckner%2C+A+S+M">Anne S. M. Buckner</a>, <a href="/search/astro-ph?searchtype=author&query=Geisler%2C+D">Douglas Geisler</a>, <a href="/search/astro-ph?searchtype=author&query=Gonzalez%2C+O+A">Oscar A. Gonzalez</a>, <a href="/search/astro-ph?searchtype=author&query=Gran%2C+F">Felipe Gran</a> , et al. (13 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="1703.02033v1-abstract-short" style="display: inline;"> We use deep multi-epoch near-IR images of the VISTA Variables in the V铆a L谩ctea (VVV) Survey to search for RR Lyrae stars towards the Southern Galactic plane. Here we report the discovery of a group of RR Lyrae stars close together in VVV tile d025. Inspection of the VVV images and PSF photometry reveals that most of these stars are likely to belong to a globular cluster, that matches the position… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.02033v1-abstract-full').style.display = 'inline'; document.getElementById('1703.02033v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1703.02033v1-abstract-full" style="display: none;"> We use deep multi-epoch near-IR images of the VISTA Variables in the V铆a L谩ctea (VVV) Survey to search for RR Lyrae stars towards the Southern Galactic plane. Here we report the discovery of a group of RR Lyrae stars close together in VVV tile d025. Inspection of the VVV images and PSF photometry reveals that most of these stars are likely to belong to a globular cluster, that matches the position of the previously known star cluster FSR\,1716. The stellar density map of the field yields a $>100$ sigma detection for this candidate globular cluster, that is centered at equatorial coordinates $RA_{J2000}=$16:10:30.0, $DEC_{J2000}=-$53:44:56; and galactic coordinates $l=$329.77812, $b=-$1.59227. The color-magnitude diagram of this object reveals a well populated red giant branch, with a prominent red clump at $K_s=13.35 \pm 0.05$, and $J-K_s=1.30 \pm 0.05$. We present the cluster RR Lyrae positions, magnitudes, colors, periods and amplitudes. The presence of RR Lyrae indicates an old globular cluster, with age $>10$ Gyr. We classify this object as an Oosterhoff type I globular cluster, based on the mean period of its RR Lyrae type ab, $<P>=0.540$ days, and argue that this is a relatively metal-poor cluster with $[Fe/H] = -1.5 \pm 0.4$ dex. The mean extinction and reddening for this cluster are $A_{K_s}=0.38 \pm 0.02$, and $E(J-K_s)=0.72 \pm 0.02$ mag, respectively, as measured from the RR Lyrae colors and the near-IR color-magnitude diagram. We also measure the cluster distance using the RR Lyrae type ab stars. The cluster mean distance modulus is $(m-M)_0 = 14.38 \pm 0.03$ mag, implying a distance $D = 7.5 \pm 0.2$ kpc, and a Galactocentric distance $R_G=4.3$ kpc. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.02033v1-abstract-full').style.display = 'none'; document.getElementById('1703.02033v1-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, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages, 4 figures. ApJL, in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1703.01711">arXiv:1703.01711</a> <span> [<a href="https://arxiv.org/pdf/1703.01711">pdf</a>, <a href="https://arxiv.org/format/1703.01711">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/aa5be4">10.3847/1538-3881/aa5be4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Characterization of the VVV Survey RR Lyrae Population across the Southern Galactic Plane </p> <p class="authors"> <span class="search-hit">Authors:</span> <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">Istvan D茅k谩ny</a>, <a href="/search/astro-ph?searchtype=author&query=Majaess%2C+D">Daniel Majaess</a>, <a href="/search/astro-ph?searchtype=author&query=Palma%2C+T">Tali Palma</a>, <a href="/search/astro-ph?searchtype=author&query=Pullen%2C+J">Joyce Pullen</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">Marina Rejkuba</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=Catelan%2C+M">Marcio Catelan</a>, <a href="/search/astro-ph?searchtype=author&query=Ramos%2C+R+C">Rodrigo Contreras Ramos</a>, <a href="/search/astro-ph?searchtype=author&query=Gonzalez%2C+O+A">Oscar A. Gonzalez</a>, <a href="/search/astro-ph?searchtype=author&query=Hempel%2C+M">Maren Hempel</a>, <a href="/search/astro-ph?searchtype=author&query=Irwin%2C+M">Mike Irwin</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=Saito%2C+R+K">Roberto K. Saito</a>, <a href="/search/astro-ph?searchtype=author&query=Tissera%2C+P">Patricia Tissera</a>, <a href="/search/astro-ph?searchtype=author&query=Valenti%2C+E">Elena Valenti</a>, <a href="/search/astro-ph?searchtype=author&query=Zoccali%2C+M">Manuela Zoccali</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1703.01711v1-abstract-short" style="display: inline;"> Deep near-IR images from the VISTA Variables in the V铆a L谩ctea (VVV) Survey were used to search for RR Lyrae stars in the Southern Galactic plane. A sizable sample of 404 RR Lyrae of type ab stars was identified across a thin slice of the 4$^{\rm th}$ Galactic quadrant ($295掳< l < 350掳$, $-2.24掳< b < -1.05掳$). The sample's distance distribution exhibits a maximum density that occurs at the bulge t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.01711v1-abstract-full').style.display = 'inline'; document.getElementById('1703.01711v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1703.01711v1-abstract-full" style="display: none;"> Deep near-IR images from the VISTA Variables in the V铆a L谩ctea (VVV) Survey were used to search for RR Lyrae stars in the Southern Galactic plane. A sizable sample of 404 RR Lyrae of type ab stars was identified across a thin slice of the 4$^{\rm th}$ Galactic quadrant ($295掳< l < 350掳$, $-2.24掳< b < -1.05掳$). The sample's distance distribution exhibits a maximum density that occurs at the bulge tangent point, which implies that this primarily Oosterhoff type I population of RRab stars does not trace the bar delineated by their red clump counterparts. The bulge RR Lyrae population does not extend beyond $l \sim340 掳$, and the sample's spatial distribution presents evidence of density enhancements and substructure that warrants further investigation. Indeed, the sample may be employed to evaluate Galactic evolution models, and is particularly lucrative since half of the discovered RR Lyrae are within reach of Gaia astrometric observations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.01711v1-abstract-full').style.display = 'none'; document.getElementById('1703.01711v1-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, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 13 figures. AJ, in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1610.05707">arXiv:1610.05707</a> <span> [<a href="https://arxiv.org/pdf/1610.05707">pdf</a>, <a href="https://arxiv.org/format/1610.05707">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201628700">10.1051/0004-6361/201628700 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A machine learned classifier for RR Lyrae in the VVV survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Elorrieta%2C+F">Felipe Elorrieta</a>, <a href="/search/astro-ph?searchtype=author&query=Eyheramendy%2C+S">Susana Eyheramendy</a>, <a href="/search/astro-ph?searchtype=author&query=Jord%C3%A1n%2C+A">Andr茅s Jord谩n</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=Catelan%2C+M">M谩rcio Catelan</a>, <a href="/search/astro-ph?searchtype=author&query=Angeloni%2C+R">Rodolfo Angeloni</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=Contreras-Ramos%2C+R">Rodrigo Contreras-Ramos</a>, <a href="/search/astro-ph?searchtype=author&query=Gran%2C+F">Felipe Gran</a>, <a href="/search/astro-ph?searchtype=author&query=Hajdu%2C+G">Gergely Hajdu</a>, <a href="/search/astro-ph?searchtype=author&query=Espinoza%2C+N">N茅stor Espinoza</a>, <a href="/search/astro-ph?searchtype=author&query=Saito%2C+R+K">Roberto K. Saito</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">Dante Minniti</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1610.05707v1-abstract-short" style="display: inline;"> Variable stars of RR Lyrae type are a prime tool to obtain distances to old stellar populations in the Milky Way, and one of the main aims of the Vista Variables in the Via Lactea (VVV) near-infrared survey is to use them to map the structure of the Galactic Bulge. Due to the large number of expected sources, this requires an automated mechanism for selecting RR Lyrae,and particularly those of the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1610.05707v1-abstract-full').style.display = 'inline'; document.getElementById('1610.05707v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1610.05707v1-abstract-full" style="display: none;"> Variable stars of RR Lyrae type are a prime tool to obtain distances to old stellar populations in the Milky Way, and one of the main aims of the Vista Variables in the Via Lactea (VVV) near-infrared survey is to use them to map the structure of the Galactic Bulge. Due to the large number of expected sources, this requires an automated mechanism for selecting RR Lyrae,and particularly those of the more easily recognized type ab (i.e., fundamental-mode pulsators), from the 10^6-10^7 variables expected in the VVV survey area. In this work we describe a supervised machine-learned classifier constructed for assigning a score to a K_s-band VVV light curve that indicates its likelihood of being ab-type RR Lyrae. We describe the key steps in the construction of the classifier, which were the choice of features, training set, selection of aperture and family of classifiers. We find that the AdaBoost family of classifiers give consistently the best performance for our problem, and obtain a classifier based on the AdaBoost algorithm that achieves a harmonic mean between false positives and false negatives of ~7% for typical VVV light curve sets. This performance is estimated using cross-validation and through the comparison to two independent datasets that were classified by human experts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1610.05707v1-abstract-full').style.display = 'none'; document.getElementById('1610.05707v1-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 October, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 7 figures. Astronomy & Astrophysics, in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1607.08623">arXiv:1607.08623</a> <span> [<a href="https://arxiv.org/pdf/1607.08623">pdf</a>, <a href="https://arxiv.org/ps/1607.08623">ps</a>, <a href="https://arxiv.org/format/1607.08623">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/10.1051/0004-6361/201628763">10.1051/0004-6361/201628763 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraining Dust Extinction Properties via the VVV Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Majaess%2C+D">D. Majaess</a>, <a href="/search/astro-ph?searchtype=author&query=Turner%2C+D">D. Turner</a>, <a href="/search/astro-ph?searchtype=author&query=Dekany%2C+I">I. Dekany</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Gieren%2C+W">W. Gieren</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="1607.08623v1-abstract-short" style="display: inline;"> Near-infrared color-excess and extinction ratios are essential for establishing the cosmic distance scale and probing the Galaxy, particularly when analyzing targets attenuated by significant dust. A robust determination of those ratios followed from leveraging new infrared observations from the VVV survey, wherein numerous bulge RR Lyrae and Type II Cepheids were discovered, in addition to… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1607.08623v1-abstract-full').style.display = 'inline'; document.getElementById('1607.08623v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1607.08623v1-abstract-full" style="display: none;"> Near-infrared color-excess and extinction ratios are essential for establishing the cosmic distance scale and probing the Galaxy, particularly when analyzing targets attenuated by significant dust. A robust determination of those ratios followed from leveraging new infrared observations from the VVV survey, wherein numerous bulge RR Lyrae and Type II Cepheids were discovered, in addition to $BVJHK_{s}(3.4\rightarrow22)渭m$ data for classical Cepheids and O-stars occupying the broader Galaxy. The apparent optical color-excess ratios vary significantly with Galactic longitude ($\ell$), whereas the near-infrared results are comparatively constant with $\ell$ and Galactocentric distance ($\langle E(J-\overline{3.5渭m})/E(J-K_s) \rangle =1.28\pm0.03$). The results derived imply that classical Cepheids and O-stars display separate optical trends ($R_{V,BV}$) with $\ell$, which appear to disfavor theories advocating a strict and marked decrease in dust size with increasing Galactocentric distance. The classical Cepheid, Type II Cepheid, and RR Lyrae variables are characterized by $\langle A_{J}/E(J-K_s) \rangle = \langle R_{J,JK_s} \rangle =1.49\pm0.05$ ($\langle A_{K_s}/A_J \rangle =0.33\pm0.02$), whereas the O-stars are expectedly impacted by emission beyond $3.6 渭m$. The mean optical ratios characterizing classical Cepheids and O-stars are approximately $\langle R_{V,BV} \rangle \sim3.1$ and $\langle R_{V,BV} \rangle \sim3.3$, respectively. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1607.08623v1-abstract-full').style.display = 'none'; document.getElementById('1607.08623v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 July, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">To appear in Astronomy and Astrophysics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1607.05286">arXiv:1607.05286</a> <span> [<a href="https://arxiv.org/pdf/1607.05286">pdf</a>, <a href="https://arxiv.org/format/1607.05286">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stw1674">10.1093/mnras/stw1674 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Near-infrared photometry and spectroscopy of the low Galactic latitude globular cluster 2MASS-GC03 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Carballo-Bello%2C+J+A">Julio A. Carballo-Bello</a>, <a href="/search/astro-ph?searchtype=author&query=Alegria%2C+S+R">S. Ramirez Alegria</a>, <a href="/search/astro-ph?searchtype=author&query=Borissova%2C+J">J. Borissova</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+L+C">L. C. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtev%2C+R">R. Kurtev</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=Bidin%2C+C+M">Ch. Moni Bidin</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=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Palma%2C+T">T. Palma</a>, <a href="/search/astro-ph?searchtype=author&query=Dekany%2C+I">I. Dekany</a>, <a href="/search/astro-ph?searchtype=author&query=Medina%2C+N">N. Medina</a>, <a href="/search/astro-ph?searchtype=author&query=Moyano%2C+M">M. Moyano</a>, <a href="/search/astro-ph?searchtype=author&query=Villanueva%2C+V">V. Villanueva</a>, <a href="/search/astro-ph?searchtype=author&query=Kuhn%2C+M+A">M. A. Kuhn</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="1607.05286v1-abstract-short" style="display: inline;"> We present deep near-infrared photometry and spectroscopy of the globular cluster 2MASS-GC03 projected in the Galactic disk using MMIRS on the Clay telescope (Las Campanas Observatory) and VISTA Variables in the Via Lactea survey (VVV) data. Most probable cluster member candidates were identified from near-infrared photometry. Out of ten candidates that were followed-up spectroscopically, five hav… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1607.05286v1-abstract-full').style.display = 'inline'; document.getElementById('1607.05286v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1607.05286v1-abstract-full" style="display: none;"> We present deep near-infrared photometry and spectroscopy of the globular cluster 2MASS-GC03 projected in the Galactic disk using MMIRS on the Clay telescope (Las Campanas Observatory) and VISTA Variables in the Via Lactea survey (VVV) data. Most probable cluster member candidates were identified from near-infrared photometry. Out of ten candidates that were followed-up spectroscopically, five have properties of cluster members, from which we calculate <[Fe/H]> = -0.9 +- 0.2 and a radial velocity of v_r > = -78 +- 12km/s. A distance of 10.8kpc is estimated from 3 likely RRLyrae members. Given that the cluster is currently at a distance of 4.2kpc from the Galactic center, the cluster's long survival time of an estimated 11.3 +- 1.2Gyr strengthens the case for its globular-cluster nature. The cluster has a hint of elongation in the direction of the Galactic center. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1607.05286v1-abstract-full').style.display = 'none'; document.getElementById('1607.05286v1-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 July, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication, 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/1607.01795">arXiv:1607.01795</a> <span> [<a href="https://arxiv.org/pdf/1607.01795">pdf</a>, <a href="https://arxiv.org/ps/1607.01795">ps</a>, <a href="https://arxiv.org/format/1607.01795">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stw1613">10.1093/mnras/stw1613 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Variable Stars in the Quintuplet stellar cluster with the VVV Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Molina%2C+C+N">C. Navarro Molina</a>, <a href="/search/astro-ph?searchtype=author&query=Borissova%2C+J">J. Borissova</a>, <a href="/search/astro-ph?searchtype=author&query=Catelan%2C+M">M. Catelan</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=Kerins%2C+E">E. Kerins</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtev%2C+R">R. Kurtev</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=Medina%2C+N">N. Medina</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%A9k%C3%A1ny%2C+I">I. D茅k谩ny</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="1607.01795v2-abstract-short" style="display: inline;"> The Quintuplet cluster is one of the most massive star clusters in the Milky Way, situated very close to the Galactic center. We present a new search for variable stars in the vicinity of the cluster, using the five-year database of the Vista Variables in the Via Lactea (VVV) ESO Public Survey in the near-infrared. A total of 7586 objects were identified in the zone around $2'$ from the cluster ce… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1607.01795v2-abstract-full').style.display = 'inline'; document.getElementById('1607.01795v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1607.01795v2-abstract-full" style="display: none;"> The Quintuplet cluster is one of the most massive star clusters in the Milky Way, situated very close to the Galactic center. We present a new search for variable stars in the vicinity of the cluster, using the five-year database of the Vista Variables in the Via Lactea (VVV) ESO Public Survey in the near-infrared. A total of 7586 objects were identified in the zone around $2'$ from the cluster center, using 55 $K_S$-band epochs. Thirty-three stars show $K_S$-band variability, 24 of them being previously undiscovered. Most of the variable stars found are slow/semiregular variables, long-period variables of the Mira type, and OH/IR stars. In addition, a good number of our candidates show variations in a rather short timescale. We also propose four Young Stellar Object (YSO) candidates, which could be cluster members. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1607.01795v2-abstract-full').style.display = 'none'; document.getElementById('1607.01795v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 July, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 July, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 10 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/1606.05028">arXiv:1606.05028</a> <span> [<a href="https://arxiv.org/pdf/1606.05028">pdf</a>, <a href="https://arxiv.org/format/1606.05028">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/10.1016/j.newast.2016.05.008">10.1016/j.newast.2016.05.008 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> New variable stars discovered in the fields of three Galactic open clusters using the VVV Survey </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=Minniti%2C+D">Dante Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%A9k%C3%A1ny%2C+I">Istvan D茅k谩ny</a>, <a href="/search/astro-ph?searchtype=author&query=Clari%C3%A1%2C+J+J">Juan J. Clari谩</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=Gramajo%2C+L+V">Luciana V. Gramajo</a>, <a href="/search/astro-ph?searchtype=author&query=Alegr%C3%ADa%2C+S+R">Sebastian Ram铆rez Alegr铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Bonatto%2C+C">Charles Bonatto</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1606.05028v1-abstract-short" style="display: inline;"> This project is a massive near-infrared (NIR) search for variable stars in highly reddened and obscured open cluster (OC) fields projected on regions of the Galactic bulge and disk. The search is performed using photometric NIR data in the $J$-, $H$- and $K_s$- bands obtained from the Vista Variables in the V铆a L谩ctea (VVV) Survey. We performed in each cluster field a variability search using Stet… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1606.05028v1-abstract-full').style.display = 'inline'; document.getElementById('1606.05028v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1606.05028v1-abstract-full" style="display: none;"> This project is a massive near-infrared (NIR) search for variable stars in highly reddened and obscured open cluster (OC) fields projected on regions of the Galactic bulge and disk. The search is performed using photometric NIR data in the $J$-, $H$- and $K_s$- bands obtained from the Vista Variables in the V铆a L谩ctea (VVV) Survey. We performed in each cluster field a variability search using Stetson's variability statistics to select the variable candidates. Later, those candidates were subjected to a frequency analysis using the Generalized Lomb-Scargle and the Phase Dispersion Minimization algorithms. The number of independent observations range between 63 and 73. The newly discovered variables in this study, 157 in total in three different known OCs, are classified based on their light curve shapes, periods, amplitudes and their location in the corresponding color-magnitude $(J-K_s,K_s)$ and color-color $(H-K_s,J-H)$ diagrams. We found 5 possible Cepheid stars which, based on the period-luminosity relation, are very likely type II Cepheids located behind the bulge. Among the newly discovered variables, there are eclipsing binaries, $未$ Scuti, as well as background RR Lyrae stars. Using the new version of the Wilson & Devinney code as well as the "Physics Of Eclipsing Binaries" (PHOEBE) code, we analyzed some of the best eclipsing binaries we discovered. Our results show that these studied systems turn out to be ranging from detached to double-contact binaries, with low eccentricities and high inclinations of approximately $80^{\circ}$. Their surface temperatures range between $3500$K and $8000$K. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1606.05028v1-abstract-full').style.display = 'none'; document.getElementById('1606.05028v1-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 June, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">34 pages, 10 figures, 7 tables. Accepted for publication in New Astronomy</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1509.08402">arXiv:1509.08402</a> <span> [<a href="https://arxiv.org/pdf/1509.08402">pdf</a>, <a href="https://arxiv.org/format/1509.08402">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/10.1088/2041-8205/812/2/L29">10.1088/2041-8205/812/2/L29 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The VVV Survey reveals classical Cepheids tracing a young and thin stellar disk across the Galaxy's bulge </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Majaess%2C+D">D. Majaess</a>, <a href="/search/astro-ph?searchtype=author&query=Zoccali%2C+M">M. Zoccali</a>, <a href="/search/astro-ph?searchtype=author&query=Hajdu%2C+G">G. Hajdu</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=Catelan%2C+M">M. Catelan</a>, <a href="/search/astro-ph?searchtype=author&query=Gieren%2C+W">W. Gieren</a>, <a href="/search/astro-ph?searchtype=author&query=Borissova%2C+J">J. Borissova</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="1509.08402v1-abstract-short" style="display: inline;"> Solid insight into the physics of the inner Milky Way is key to understanding our Galaxy's evolution, but extreme dust obscuration has historically hindered efforts to map the area along the Galactic mid-plane. New comprehensive near-infrared time-series photometry from the VVV Survey has revealed 35 classical Cepheids, tracing a previously unobserved component of the inner Galaxy, namely a ubiqui… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.08402v1-abstract-full').style.display = 'inline'; document.getElementById('1509.08402v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1509.08402v1-abstract-full" style="display: none;"> Solid insight into the physics of the inner Milky Way is key to understanding our Galaxy's evolution, but extreme dust obscuration has historically hindered efforts to map the area along the Galactic mid-plane. New comprehensive near-infrared time-series photometry from the VVV Survey has revealed 35 classical Cepheids, tracing a previously unobserved component of the inner Galaxy, namely a ubiquitous inner thin disk of young stars along the Galactic mid-plane, traversing across the bulge. The discovered period (age) spread of these classical Cepheids implies a continuous supply of newly formed stars in the central region of the Galaxy over the last 100 million years. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.08402v1-abstract-full').style.display = 'none'; document.getElementById('1509.08402v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 September, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in The Astrophysical Journal Letters. Near-IR finding charts of the Cepheids are available at the following URL: http://www.astro.puc.cl/~idekany/pub/inner_disk_ceph_fc.png</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1502.01318">arXiv:1502.01318</a> <span> [<a href="https://arxiv.org/pdf/1502.01318">pdf</a>, <a href="https://arxiv.org/ps/1502.01318">ps</a>, <a href="https://arxiv.org/format/1502.01318">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnrasl/slv024">10.1093/mnrasl/slv024 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> New RR Lyrae variables in binary systems </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hajdu%2C+G">G. Hajdu</a>, <a href="/search/astro-ph?searchtype=author&query=Catelan%2C+M">M. Catelan</a>, <a href="/search/astro-ph?searchtype=author&query=Jurcsik%2C+J">J. Jurcsik</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=Drake%2C+A+J">A. J. Drake</a>, <a href="/search/astro-ph?searchtype=author&query=Marquette%2C+J+-">J. -B. Marquette</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="1502.01318v1-abstract-short" style="display: inline;"> Despite their importance, very few RR Lyrae (RRL) stars have been known to reside in binary systems. We report on a search for binary RRL in the OGLE-III Galactic bulge data. Our approach consists in the search for evidence of the light-travel time effect in so-called observed minus calculated ($O-C$) diagrams. Analysis of 1952 well-observed fundamental-mode RRL in the OGLE-III data revealed an in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1502.01318v1-abstract-full').style.display = 'inline'; document.getElementById('1502.01318v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1502.01318v1-abstract-full" style="display: none;"> Despite their importance, very few RR Lyrae (RRL) stars have been known to reside in binary systems. We report on a search for binary RRL in the OGLE-III Galactic bulge data. Our approach consists in the search for evidence of the light-travel time effect in so-called observed minus calculated ($O-C$) diagrams. Analysis of 1952 well-observed fundamental-mode RRL in the OGLE-III data revealed an initial sample of 29 candidates. We used the recently released OGLE-IV data to extend the baselines up to 17 years, leading to a final sample of 12 firm binary candidates. We provide $O-C$ diagrams and binary parameters for this final sample, and also discuss the properties of 8 additional candidate binaries whose parameters cannot be firmly determined at present. We also estimate that $\gtrsim 4$ per cent of the RRL reside in binary systems. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1502.01318v1-abstract-full').style.display = 'none'; document.getElementById('1502.01318v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 February, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">MNRAS Letters, in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1501.02286">arXiv:1501.02286</a> <span> [<a href="https://arxiv.org/pdf/1501.02286">pdf</a>, <a href="https://arxiv.org/format/1501.02286">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201424838">10.1051/0004-6361/201424838 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An Updated Census of RR~Lyrae Stars in the Globular Cluster $蠅$~Centauri (NGC\,5139) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Navarrete%2C+C">C. Navarrete</a>, <a href="/search/astro-ph?searchtype=author&query=Ramos%2C+R+C">R. Contreras Ramos</a>, <a href="/search/astro-ph?searchtype=author&query=Catelan%2C+M">M. Catelan</a>, <a href="/search/astro-ph?searchtype=author&query=Clement%2C+C+M">C. M. Clement</a>, <a href="/search/astro-ph?searchtype=author&query=Gran%2C+F">F. Gran</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=Angeloni%2C+R">R. Angeloni</a>, <a href="/search/astro-ph?searchtype=author&query=Hempel%2C+M">M. Hempel</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=Minniti%2C+D">D. Minniti</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1501.02286v1-abstract-short" style="display: inline;"> [ABRIDGED] $蠅$ Centauri (NGC 5139) contains large numbers of variable stars of different types and, in particular, more than a hundred RR Lyrae stars. We have conducted a variability survey of $蠅$ Cen in the NIR, using ESO's 4.1m Visible and Infrared Survey Telescope for Astronomy (VISTA). This is the first paper of a series describing our results. $蠅$ Cen was observed using VIRCAM mounted on VI… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1501.02286v1-abstract-full').style.display = 'inline'; document.getElementById('1501.02286v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1501.02286v1-abstract-full" style="display: none;"> [ABRIDGED] $蠅$ Centauri (NGC 5139) contains large numbers of variable stars of different types and, in particular, more than a hundred RR Lyrae stars. We have conducted a variability survey of $蠅$ Cen in the NIR, using ESO's 4.1m Visible and Infrared Survey Telescope for Astronomy (VISTA). This is the first paper of a series describing our results. $蠅$ Cen was observed using VIRCAM mounted on VISTA. A total of 42 and 100 epochs in $J$ and $K_{\rm S}$, respectively, were obtained, distributed over a total timespan of 352 days. PSF photometry was performed, and periods of the known variable stars were improved when necessary using an ANOVA analysis. An unprecedented homogeneous and complete NIR catalogue of RR Lyrae stars in the field of $蠅$ Cen was collected, allowing us to study, for the first time, all the RR Lyrae stars associated to the cluster, except 4 located far away from the cluster center. Membership status, subclassifications between RRab and RRc subtypes, periods, amplitudes, and mean magnitudes were derived for all the stars in our sample. Additionally, 4 new RR Lyrae stars were discovered, 2 of them with high probability of being cluster members. The distribution of $蠅$ Cen stars in the Bailey (period-amplitude) diagram is also discussed. Reference lines in this plane, for both Oosterhoff type I (OoI) and II (OoII) components, are provided. In the present paper, we clarify the status of many (candidate) RR Lyrae stars that had been unclear in previous studies. This includes stars with anomalous positions in the color-magnitude diagram, uncertain periods or/and variability types, and possible field interlopers. We conclude that $蠅$ Cen hosts a total of 88 RRab and 101 RRc stars, for a grand total of 189 likely members. We confirm that most RRab stars in the cluster belong to an OoII component, as previously found using visual data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1501.02286v1-abstract-full').style.display = 'none'; document.getElementById('1501.02286v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 January, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">A\&A, in press</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 577, A99 (2015) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1501.00947">arXiv:1501.00947</a> <span> [<a href="https://arxiv.org/pdf/1501.00947">pdf</a>, <a href="https://arxiv.org/format/1501.00947">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201424333">10.1051/0004-6361/201424333 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Bulge RR Lyrae stars in the VVV tile $\textit{b201}$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gran%2C+F">F. Gran</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</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=Navarrete%2C+C">C. Navarrete</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=McDonald%2C+I">I. McDonald</a>, <a href="/search/astro-ph?searchtype=author&query=Ramos%2C+R+C">R. Contreras Ramos</a>, <a href="/search/astro-ph?searchtype=author&query=Catelan%2C+M">M. Catelan</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1501.00947v1-abstract-short" style="display: inline;"> The VISTA Variables in the V铆a L谩ctea (VVV) Survey is one of the six ESO public surveys currently ongoing at the VISTA telescope on Cerro Paranal, Chile. VVV uses near-IR ($ZYJHK_{\rm s}$) filters that at present provide photometry to a depth of $K_{\rm s} \sim 17.0$ mag in up to 36 epochs spanning over four years, and aim at discovering more than 10$^6$ variable sources as well as trace the struc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1501.00947v1-abstract-full').style.display = 'inline'; document.getElementById('1501.00947v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1501.00947v1-abstract-full" style="display: none;"> The VISTA Variables in the V铆a L谩ctea (VVV) Survey is one of the six ESO public surveys currently ongoing at the VISTA telescope on Cerro Paranal, Chile. VVV uses near-IR ($ZYJHK_{\rm s}$) filters that at present provide photometry to a depth of $K_{\rm s} \sim 17.0$ mag in up to 36 epochs spanning over four years, and aim at discovering more than 10$^6$ variable sources as well as trace the structure of the Galactic bulge and part of the southern disk. A variability search was performed to find RR Lyrae variable stars. The low stellar density of the VVV tile $\textit{b201}$, which is centered at ($\ell, b$) $\sim$ ($-9^\circ, -9^\circ$), makes it suitable to search for variable stars. Previous studies have identified some RR Lyrae stars using optical bands that served to test our search procedure. The main goal is to measure the reddening, interstellar extinction, and distances of the RR Lyrae stars and to study their distribution on the Milky Way bulge. A total of 1.5 sq deg were analyzed, and we found 39 RR Lyrae stars, 27 of which belong to the ab-type and 12 to the c-type. Our analysis recovers all the previously identified RR Lyrae variables in the field and discovers 29 new RR Lyrae stars. The reddening and extinction toward all the RRab stars in this tile were derived, and distance estimations were obtained through the period--luminosity relation. Despite the limited amount of RR Lyrae stars studied, our results are consistent with a spheroidal or central distribution around $\sim 8.1$ and $\sim 8.5$ kpc. for either the Cardelli or Nishiyama extinction law. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1501.00947v1-abstract-full').style.display = 'none'; document.getElementById('1501.00947v1-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 January, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 8 figures, accepted for publication in Astronomy and Astrophysics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1412.8658">arXiv:1412.8658</a> <span> [<a href="https://arxiv.org/pdf/1412.8658">pdf</a>, <a href="https://arxiv.org/format/1412.8658">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/2041-8205/799/1/L11">10.1088/2041-8205/799/1/L11 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery of a Pair of Classical Cepheids in an Invisible Cluster Beyond the Galactic Bulge </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Hajdu%2C+G">G. Hajdu</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=Hempel%2C+M">M. Hempel</a>, <a href="/search/astro-ph?searchtype=author&query=Palma%2C+T">T. Palma</a>, <a href="/search/astro-ph?searchtype=author&query=Catelan%2C+M">M. Catelan</a>, <a href="/search/astro-ph?searchtype=author&query=Gieren%2C+W">W. Gieren</a>, <a href="/search/astro-ph?searchtype=author&query=Majaess%2C+D">D. Majaess</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="1412.8658v1-abstract-short" style="display: inline;"> We report the discovery of a pair of extremely reddened classical Cepheid variable stars located in the Galactic plane behind the bulge, using near-infrared time-series photometry from the VVV Survey. This is the first time that such objects have ever been found in the opposite side of the Galactic plane. The Cepheids have almost identical periods, apparent brightnesses and colors. From the near-i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.8658v1-abstract-full').style.display = 'inline'; document.getElementById('1412.8658v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1412.8658v1-abstract-full" style="display: none;"> We report the discovery of a pair of extremely reddened classical Cepheid variable stars located in the Galactic plane behind the bulge, using near-infrared time-series photometry from the VVV Survey. This is the first time that such objects have ever been found in the opposite side of the Galactic plane. The Cepheids have almost identical periods, apparent brightnesses and colors. From the near-infrared Leavitt law, we determine their distances with ~1.5% precision and ~8% accuracy. We find that they have a same total extinction of A(V)~32 mag, and are located at the same heliocentric distance of <d>=11.4+/-0.9 kpc, and less than 1 pc from the true Galactic plane. Their similar periods indicate that the Cepheids are also coeval, with an age of ~48+/-3 Myr, according to theoretical models. They are separated by an angular distance of only 18.3", corresponding to a projected separation of ~1 pc. Their position coincides with the expected location of the Far 3 kpc Arm behind the bulge. Such a tight pair of similar classical Cepheids indicates the presence of an underlying young open cluster, that is both hidden behind heavy extinction and disguised by the dense stellar field of the bulge. All our attempts to directly detect this "invisible cluster" have failed, and deeper observations are needed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.8658v1-abstract-full').style.display = 'none'; document.getElementById('1412.8658v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 December, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">Accepted for publication in ApJL. Photometric data are available online at the CDS and also at http://www.astro.puc.cl/~idekany/pub/twincep.dat</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1411.1696">arXiv:1411.1696</a> <span> [<a href="https://arxiv.org/pdf/1411.1696">pdf</a>, <a href="https://arxiv.org/format/1411.1696">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-6256/149/3/99">10.1088/0004-6256/149/3/99 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Variable stars in the VVV globular clusters. I. 2MASS-GC02 and Terzan10 </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=D%C3%A9k%C3%A1ny%2C+I">Istv谩n D茅k谩ny</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=Ramos%2C+R+C">Rodrigo Contreras Ramos</a>, <a href="/search/astro-ph?searchtype=author&query=Gran%2C+F">Felipe Gran</a>, <a href="/search/astro-ph?searchtype=author&query=Amigo%2C+P">P铆a Amigo</a>, <a href="/search/astro-ph?searchtype=author&query=Leyton%2C+P">Paul Leyton</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">Dante Minniti</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1411.1696v2-abstract-short" style="display: inline;"> The VISTA Variables in the Via Lactea (VVV) ESO Public Survey is opening a new window to study the inner Galactic globular clusters using their variable stars. These globular clusters have been neglected in the past due to the difficulties caused by the presence of an elevated extinction and high field stellar densities in their lines of sight. However, the discovery and study of any present varia… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1411.1696v2-abstract-full').style.display = 'inline'; document.getElementById('1411.1696v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1411.1696v2-abstract-full" style="display: none;"> The VISTA Variables in the Via Lactea (VVV) ESO Public Survey is opening a new window to study the inner Galactic globular clusters using their variable stars. These globular clusters have been neglected in the past due to the difficulties caused by the presence of an elevated extinction and high field stellar densities in their lines of sight. However, the discovery and study of any present variables in these clusters, especially RRLyrae stars, can help to greatly improve the accuracy of their physical parameters. It can also help to shed some light on the interrogations brought by the intriguing Oosterhoff dichotomy in the Galactic globular cluster system. In a series of papers we plan to explore the variable stars in the globular clusters falling inside the field of the VVV survey. In this first paper we search and study the variables present in two highly-reddened, moderately metal-poor, faint, inner Galactic globular clusters: 2MASS-GC02 and Terzan10. We report the discovery of sizable populations of RR Lyrae stars in both globular clusters. We use near-infrared period-luminosity relations to determine the color excess of each RR Lyrae star, from which we obtain both accurate distances to the globular clusters and the ratios of the selective to total extinction in their directions. We find the extinction towards both clusters to be elevated, non-standard, and highly differential. We also find both clusters to be closer to the Galactic center than previously thought, with Terzan10 being on the far side of the Galactic bulge. Finally, we discuss their Oosterhoff properties, and conclude that both clusters stand out from the dichotomy followed by most Galactic globular clusters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1411.1696v2-abstract-full').style.display = 'none'; document.getElementById('1411.1696v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 November, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 November, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">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/1409.5836">arXiv:1409.5836</a> <span> [<a href="https://arxiv.org/pdf/1409.5836">pdf</a>, <a href="https://arxiv.org/ps/1409.5836">ps</a>, <a href="https://arxiv.org/format/1409.5836">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/10.1051/0004-6361/201424056">10.1051/0004-6361/201424056 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Milky Way demographics with the VVV Survey III. Evidence for a Great Dark Lane in the 157 Million Star Bulge Color-Magnitude Diagram </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=Saito%2C+R+K">R. K. Saito</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=Zoccali%2C+M">M. Zoccali</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">M. Rejkuba</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=Benjamin%2C+R">R. Benjamin</a>, <a href="/search/astro-ph?searchtype=author&query=Catelan%2C+M">M. Catelan</a>, <a href="/search/astro-ph?searchtype=author&query=Dekany%2C+I">I. Dekany</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=Hempel%2C+M">M. Hempel</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=Schultheis%2C+M">M. Schultheis</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="1409.5836v1-abstract-short" style="display: inline;"> The new generation of IR surveys are revealing and quantifying Galactic features, providing an improved 3-D interpretation of our own Galaxy. We present an analysis of the global distribution of dust clouds in the bulge using the near-IR photometry of 157 million stars from the VVV Survey. We investigate the color magnitude diagram of the Milky Way bulge which shows a red giant clump of core He bu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1409.5836v1-abstract-full').style.display = 'inline'; document.getElementById('1409.5836v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1409.5836v1-abstract-full" style="display: none;"> The new generation of IR surveys are revealing and quantifying Galactic features, providing an improved 3-D interpretation of our own Galaxy. We present an analysis of the global distribution of dust clouds in the bulge using the near-IR photometry of 157 million stars from the VVV Survey. We investigate the color magnitude diagram of the Milky Way bulge which shows a red giant clump of core He burning stars that is split in two color components, with a mean color difference of (Z-Ks)=0.55 magnitudes equivalent to A_V=2.0 magnitudes. We conclude that there is an optically thick dust lane at intermediate latitudes above and below the plane, that runs across several square degrees from l=-10 deg to l=+10 deg. We call this feature the "Great Dark Lane". Although its exact distance is uncertain, it is located in front of the bulge. The evidence for a large-scale great dark lane within the Galactic bulge is important in order to constrain models of the barred Milky Way bulge and to compare our galaxy with external barred galaxies, where these kinds of features are prominent. We discuss two other potential implications of the presence of the Great Dark Lane for microlensing and bulge stellar populations studies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1409.5836v1-abstract-full').style.display = 'none'; document.getElementById('1409.5836v1-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 September, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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, 4 figures, accepted for publication in Astronomy and Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 571, A91 (2014) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1408.4137">arXiv:1408.4137</a> <span> [<a href="https://arxiv.org/pdf/1408.4137">pdf</a>, <a href="https://arxiv.org/ps/1408.4137">ps</a>, <a href="https://arxiv.org/format/1408.4137">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201423793e">10.1051/0004-6361/201423793e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The WFCAM Multi-wavelength Variable Star Catalog </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lopes%2C+C+E+F">C. E. Ferreira Lopes</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=Catelan%2C+M">M. Catelan</a>, <a href="/search/astro-ph?searchtype=author&query=Cross%2C+N+J+G">N. J. G. Cross</a>, <a href="/search/astro-ph?searchtype=author&query=Angeloni%2C+R">R. Angeloni</a>, <a href="/search/astro-ph?searchtype=author&query=Le%C3%A3o%2C+I+C">I. C. Le茫o</a>, <a href="/search/astro-ph?searchtype=author&query=De+Medeiros%2C+J+R">J. R. De Medeiros</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1408.4137v3-abstract-short" style="display: inline;"> Stellar variability in the near-infrared (NIR) remains largely unexplored. The exploitation of public science archives with data-mining methods offers a perspective for the time-domain exploration of the NIR sky. We perform a comprehensive search for stellar variability using the optical-NIR multi-band photometric data in the public Calibration Database of the WFCAM Science Archive (WSA), with the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1408.4137v3-abstract-full').style.display = 'inline'; document.getElementById('1408.4137v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1408.4137v3-abstract-full" style="display: none;"> Stellar variability in the near-infrared (NIR) remains largely unexplored. The exploitation of public science archives with data-mining methods offers a perspective for the time-domain exploration of the NIR sky. We perform a comprehensive search for stellar variability using the optical-NIR multi-band photometric data in the public Calibration Database of the WFCAM Science Archive (WSA), with the aim of contributing to the general census of variable stars, and to extend the current scarce inventory of accurate NIR light curves for a number of variable star classes. We introduce new variability indices designed for multi-band data with correlated sampling, and apply them for pre-selecting variable star candidates, i.e., light curves that are dominated by correlated variations, from noise-dominated ones. Pre-selection criteria are established by robust numerical tests for evaluating the response of variability indices to colored noise characteristic to the data. We find 275 periodic variable stars and an additional 44 objects with suspected variability with uncertain periods or apparently aperiodic variation. Only 44 of these objects had been previously known, including 11 RR~Lyrae stars in the outskirts of the globular cluster M3 (NGC~5272). We provide a preliminary classification of the new variable stars that have well-measured light curves, but the variability types of a large number of objects remain ambiguous. We classify most of the new variables as contact binary stars, but we also find several pulsating stars, among which 34 are probably new field RR~Lyrae and 3 are likely Cepheids. We also identify 32 highly reddened variable objects close to previously known dark nebulae, suggesting that these are embedded young stellar objects. We publish our results and all light-curve data as the WFCAM Variable Star Catalog. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1408.4137v3-abstract-full').style.display = 'none'; document.getElementById('1408.4137v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 September, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 August, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 11 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 580, C3 (2015) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1406.6727">arXiv:1406.6727</a> <span> [<a href="https://arxiv.org/pdf/1406.6727">pdf</a>, <a href="https://arxiv.org/ps/1406.6727">ps</a>, <a href="https://arxiv.org/format/1406.6727">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Stellar Variability in the VVV Survey: An Update </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Catelan%2C+M">M. Catelan</a>, <a href="/search/astro-ph?searchtype=author&query=Dekany%2C+I">I. Dekany</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> </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="1406.6727v1-abstract-short" style="display: inline;"> The Vista Variables in the Via Lactea (VVV) ESO Public Survey consists in a near-infrared time-series survey of the Galactic bulge and inner disk, covering 562 square degrees of the sky, over a total timespan of more than 5 years. In this paper, we provide an updated account of the current status of the survey, especially in the context of stellar variability studies. In this sense, we give a firs… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1406.6727v1-abstract-full').style.display = 'inline'; document.getElementById('1406.6727v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1406.6727v1-abstract-full" style="display: none;"> The Vista Variables in the Via Lactea (VVV) ESO Public Survey consists in a near-infrared time-series survey of the Galactic bulge and inner disk, covering 562 square degrees of the sky, over a total timespan of more than 5 years. In this paper, we provide an updated account of the current status of the survey, especially in the context of stellar variability studies. In this sense, we give a first description of our efforts towards the construction of the VVV Variable Star Catalog (VVV-VSC). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1406.6727v1-abstract-full').style.display = 'none'; document.getElementById('1406.6727v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 June, 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">10 pages, 6 figures. Invited review, to appear in BAAA (Boletin de la Asociacion Argentina de Astronomia)</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/1405.4517">arXiv:1405.4517</a> <span> [<a href="https://arxiv.org/pdf/1405.4517">pdf</a>, <a href="https://arxiv.org/ps/1405.4517">ps</a>, <a href="https://arxiv.org/format/1405.4517">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201423904">10.1051/0004-6361/201423904 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The VVV Templates Project. Towards an Automated Classification of VVV Light-Curves. I. Building a database of stellar variability in the near-infrared </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Angeloni%2C+R">R. Angeloni</a>, <a href="/search/astro-ph?searchtype=author&query=Ramos%2C+R+C">R. Contreras Ramos</a>, <a href="/search/astro-ph?searchtype=author&query=Catelan%2C+M">M. Catelan</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=Gran%2C+F">F. Gran</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=Hempel%2C+M">M. Hempel</a>, <a href="/search/astro-ph?searchtype=author&query=Navarrete%2C+C">C. Navarrete</a>, <a href="/search/astro-ph?searchtype=author&query=Andrews%2C+H">H. Andrews</a>, <a href="/search/astro-ph?searchtype=author&query=Aparicio%2C+A">A. Aparicio</a>, <a href="/search/astro-ph?searchtype=author&query=Beam%C3%ADn%2C+J+C">J. C. Beam铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+C">C. Berger</a>, <a href="/search/astro-ph?searchtype=author&query=Borissova%2C+J">J. Borissova</a>, <a href="/search/astro-ph?searchtype=author&query=Pe%C3%B1a%2C+C+C">C. Contreras Pe帽a</a>, <a href="/search/astro-ph?searchtype=author&query=Cunial%2C+A">A. Cunial</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=Espinoza%2C+N">N. Espinoza</a>, <a href="/search/astro-ph?searchtype=author&query=Eyheramendy%2C+S">S. Eyheramendy</a>, <a href="/search/astro-ph?searchtype=author&query=Lopes%2C+C+E+F">C. E. Ferreira Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Fiaschi%2C+M">M. Fiaschi</a>, <a href="/search/astro-ph?searchtype=author&query=Hajdu%2C+G">G. Hajdu</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+J">J. Han</a>, <a href="/search/astro-ph?searchtype=author&query=He%C5%82miniak%2C+K+G">K. G. He艂miniak</a>, <a href="/search/astro-ph?searchtype=author&query=Hempel%2C+A">A. Hempel</a>, <a href="/search/astro-ph?searchtype=author&query=Hidalgo%2C+S+L">S. L. Hidalgo</a> , et al. (28 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="1405.4517v2-abstract-short" style="display: inline;"> Context. The Vista Variables in the V铆a L谩ctea (VVV) ESO Public Survey is a variability survey of the Milky Way bulge and an adjacent section of the disk carried out from 2010 on ESO Visible and Infrared Survey Telescope for Astronomy (VISTA). VVV will eventually deliver a deep near-IR atlas with photometry and positions in five passbands (ZYJHK_S) and a catalogue of 1-10 million variable point so… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1405.4517v2-abstract-full').style.display = 'inline'; document.getElementById('1405.4517v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1405.4517v2-abstract-full" style="display: none;"> Context. The Vista Variables in the V铆a L谩ctea (VVV) ESO Public Survey is a variability survey of the Milky Way bulge and an adjacent section of the disk carried out from 2010 on ESO Visible and Infrared Survey Telescope for Astronomy (VISTA). VVV will eventually deliver a deep near-IR atlas with photometry and positions in five passbands (ZYJHK_S) and a catalogue of 1-10 million variable point sources - mostly unknown - which require classifications. Aims. The main goal of the VVV Templates Project, that we introduce in this work, is to develop and test the machine-learning algorithms for the automated classification of the VVV light-curves. As VVV is the first massive, multi-epoch survey of stellar variability in the near-infrared, the template light-curves that are required for training the classification algorithms are not available. In the first paper of the series we describe the construction of this comprehensive database of infrared stellar variability. Methods. First we performed a systematic search in the literature and public data archives, second, we coordinated a worldwide observational campaign, and third we exploited the VVV variability database itself on (optically) well-known stars to gather high-quality infrared light-curves of several hundreds of variable stars. Results. We have now collected a significant (and still increasing) number of infrared template light-curves. This database will be used as a training-set for the machine-learning algorithms that will automatically classify the light-curves produced by VVV. The results of such an automated classification will be covered in forthcoming papers of the series. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1405.4517v2-abstract-full').style.display = 'none'; document.getElementById('1405.4517v2-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, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 May, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 16 figures, 3 tables, accepted for publication in A&A. Most of the data are now accessible through http://www.vvvtemplates.org/</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 567, A100 (2014) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1312.3951">arXiv:1312.3951</a> <span> [<a href="https://arxiv.org/pdf/1312.3951">pdf</a>, <a href="https://arxiv.org/format/1312.3951">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/785/2/155">10.1088/0004-637X/785/2/155 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Sub-Earth-Mass Moon Orbiting a Gas Giant Primary or a High Velocity Planetary System in the Galactic Bulge </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+D+P">D. P. Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+V">V. Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+I+A">I. A. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+C+S">C. S. Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Suzuki%2C+D">D. Suzuki</a>, <a href="/search/astro-ph?searchtype=author&query=Beaulieu%2C+J+-">J. -P. Beaulieu</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">A. Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Donatowicz%2C+J">J. Donatowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+F">F. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Botzler%2C+C+S">C. S. Botzler</a>, <a href="/search/astro-ph?searchtype=author&query=Freeman%2C+M">M. Freeman</a>, <a href="/search/astro-ph?searchtype=author&query=Fukunaga%2C+D">D. Fukunaga</a>, <a href="/search/astro-ph?searchtype=author&query=Fukui%2C+A">A. Fukui</a>, <a href="/search/astro-ph?searchtype=author&query=Itow%2C+Y">Y. Itow</a>, <a href="/search/astro-ph?searchtype=author&query=Koshimoto%2C+N">N. Koshimoto</a>, <a href="/search/astro-ph?searchtype=author&query=Ling%2C+C+H">C. H. Ling</a>, <a href="/search/astro-ph?searchtype=author&query=Masuda%2C+K">K. Masuda</a>, <a href="/search/astro-ph?searchtype=author&query=Matsubara%2C+Y">Y. Matsubara</a>, <a href="/search/astro-ph?searchtype=author&query=Muraki%2C+Y">Y. Muraki</a>, <a href="/search/astro-ph?searchtype=author&query=Namba%2C+S">S. Namba</a>, <a href="/search/astro-ph?searchtype=author&query=Ohnishi%2C+K">K. Ohnishi</a>, <a href="/search/astro-ph?searchtype=author&query=Rattenbury%2C+N+J">N. J. Rattenbury</a>, <a href="/search/astro-ph?searchtype=author&query=Saito%2C+T">To. Saito</a>, <a href="/search/astro-ph?searchtype=author&query=Sullivan%2C+D+J">D. J. Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=Sumi%2C+T">T. Sumi</a> , et al. (68 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1312.3951v1-abstract-short" style="display: inline;"> We present the first microlensing candidate for a free-floating exoplanet-exomoon system, MOA-2011-BLG-262, with a primary lens mass of M_host ~ 4 Jupiter masses hosting a sub-Earth mass moon. The data are well fit by this exomoon model, but an alternate star+planet model fits the data almost as well. Nevertheless, these results indicate the potential of microlensing to detect exomoons, albeit one… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1312.3951v1-abstract-full').style.display = 'inline'; document.getElementById('1312.3951v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1312.3951v1-abstract-full" style="display: none;"> We present the first microlensing candidate for a free-floating exoplanet-exomoon system, MOA-2011-BLG-262, with a primary lens mass of M_host ~ 4 Jupiter masses hosting a sub-Earth mass moon. The data are well fit by this exomoon model, but an alternate star+planet model fits the data almost as well. Nevertheless, these results indicate the potential of microlensing to detect exomoons, albeit ones that are different from the giant planet moons in our solar system. The argument for an exomoon hinges on the system being relatively close to the Sun. The data constrain the product M pi_rel, where M is the lens system mass and pi_rel is the lens-source relative parallax. If the lens system is nearby (large pi_rel), then M is small (a few Jupiter masses) and the companion is a sub-Earth-mass exomoon. The best-fit solution has a large lens-source relative proper motion, mu_rel = 19.6 +- 1.6 mas/yr, which would rule out a distant lens system unless the source star has an unusually high proper motion. However, data from the OGLE collaboration nearly rule out a high source proper motion, so the exoplanet+exomoon model is the favored interpretation for the best fit model. However, the alternate solution has a lower proper motion, which is compatible with a distant (so stellar) host. A Bayesian analysis does not favor the exoplanet+exomoon interpretation, so Occam's razor favors a lens system in the bulge with host and companion masses of M_host = 0.12 (+0.19 -0.06) M_solar and m_comp = 18 (+28 -100 M_earth, at a projected separation of a_perp ~ 0.84 AU. The existence of this degeneracy is an unlucky accident, so current microlensing experiments are in principle sensitive to exomoons. In some circumstances, it will be possible to definitively establish the low mass of such lens systems through the microlensing parallax effect. Future experiments will be sensitive to less extreme exomoons. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1312.3951v1-abstract-full').style.display = 'none'; document.getElementById('1312.3951v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 December, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">32 pages with 9 included figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1310.1996">arXiv:1310.1996</a> <span> [<a href="https://arxiv.org/pdf/1310.1996">pdf</a>, <a href="https://arxiv.org/ps/1310.1996">ps</a>, <a href="https://arxiv.org/format/1310.1996">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Stellar Variability in the VVV survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <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+W">P. W. Lucas</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=Saito%2C+R+K">R. K. Saito</a>, <a href="/search/astro-ph?searchtype=author&query=Angeloni%2C+R">R. Angeloni</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=Hempel%2C+M">M. Hempel</a>, <a href="/search/astro-ph?searchtype=author&query=Helminiak%2C+K">K. Helminiak</a>, <a href="/search/astro-ph?searchtype=author&query=Jord%C3%A1n%2C+A">A. Jord谩n</a>, <a href="/search/astro-ph?searchtype=author&query=Ramos%2C+R+C">R. Contreras Ramos</a>, <a href="/search/astro-ph?searchtype=author&query=Navarrete%2C+C">C. Navarrete</a>, <a href="/search/astro-ph?searchtype=author&query=Beam%C3%ADn%2C+J+C">J. C. Beam铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas%2C+A+F">A. F. Rojas</a>, <a href="/search/astro-ph?searchtype=author&query=Gran%2C+F">F. Gran</a>, <a href="/search/astro-ph?searchtype=author&query=Lopes%2C+C+E+F">C. E. Ferreira Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Pe%C3%B1a%2C+C+C">C. Contreras Pe帽a</a>, <a href="/search/astro-ph?searchtype=author&query=Kerins%2C+E">E. Kerins</a>, <a href="/search/astro-ph?searchtype=author&query=Huckvale%2C+L">L. Huckvale</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">M. Rejkuba</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R">R. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Mauro%2C+F">F. Mauro</a>, <a href="/search/astro-ph?searchtype=author&query=Borissova%2C+J">J. Borissova</a>, <a href="/search/astro-ph?searchtype=author&query=Amigo%2C+P">P. Amigo</a>, <a href="/search/astro-ph?searchtype=author&query=Eyheramendy%2C+S">S. Eyheramendy</a> , et al. (12 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="1310.1996v2-abstract-short" style="display: inline;"> The Vista Variables in the V铆a L谩ctea (VVV) ESO Public Survey is an ongoing time-series, near-infrared (IR) survey of the Galactic bulge and an adjacent portion of the inner disk, covering 562 square degrees of the sky, using ESO's VISTA telescope. The survey has provided superb multi-color photometry in 5 broadband filters ($Z$, $Y$, $J$, $H$, and $K_s$), leading to the best map of the inner Milk… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1310.1996v2-abstract-full').style.display = 'inline'; document.getElementById('1310.1996v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1310.1996v2-abstract-full" style="display: none;"> The Vista Variables in the V铆a L谩ctea (VVV) ESO Public Survey is an ongoing time-series, near-infrared (IR) survey of the Galactic bulge and an adjacent portion of the inner disk, covering 562 square degrees of the sky, using ESO's VISTA telescope. The survey has provided superb multi-color photometry in 5 broadband filters ($Z$, $Y$, $J$, $H$, and $K_s$), leading to the best map of the inner Milky Way ever obtained, particularly in the near-IR. The main variability part of the survey, which is focused on $K_s$-band observations, is currently underway, with bulge fields having been observed between 31 and 70 times, and disk fields between 17 and 36 times. When the survey is complete, bulge (disk) fields will have been observed up to a total of 100 (60) times, providing unprecedented depth and time coverage. Here we provide a first overview of stellar variability in the VVV data, including examples of the light curves that have been collected thus far, scientific applications, and our efforts towards the automated classification of VVV light curves. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1310.1996v2-abstract-full').style.display = 'none'; document.getElementById('1310.1996v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 November, 2013; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 October, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">Presented at the "40 Years of Variable Stars: A Celebration of Contributions by Horace A. Smith" conference (arXiv:1310.0149). 49 pages, 28 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> HASMITH/2013/17 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1309.5933">arXiv:1309.5933</a> <span> [<a href="https://arxiv.org/pdf/1309.5933">pdf</a>, <a href="https://arxiv.org/format/1309.5933">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/10.1088/2041-8205/776/2/L19">10.1088/2041-8205/776/2/L19 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> VVV Survey Near-Infrared Photometry of Known Bulge RR Lyrae stars: the Distance to the Galactic Center and Absence of a Barred Distribution of the Metal-Poor Population </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Catelan%2C+M">M. Catelan</a>, <a href="/search/astro-ph?searchtype=author&query=Zoccali%2C+M">M. Zoccali</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=Gonzalez%2C+O+A">O. A. Gonzalez</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="1309.5933v1-abstract-short" style="display: inline;"> We have combined optical and near-infrared data of known RR Lyrae (RRL) stars in the bulge in order to study the spatial distribution of its metal-poor component by measuring precise reddening values and distances of 7663 fundamental-mode RRL stars with high-quality photometry. We obtain a distance to the Galactic center of R0 = 8.33 +/- 0.05 +/- 0.14 kpc. We find that the spatial distribution of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1309.5933v1-abstract-full').style.display = 'inline'; document.getElementById('1309.5933v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1309.5933v1-abstract-full" style="display: none;"> We have combined optical and near-infrared data of known RR Lyrae (RRL) stars in the bulge in order to study the spatial distribution of its metal-poor component by measuring precise reddening values and distances of 7663 fundamental-mode RRL stars with high-quality photometry. We obtain a distance to the Galactic center of R0 = 8.33 +/- 0.05 +/- 0.14 kpc. We find that the spatial distribution of the RRL stars differs from the structures traced by the predominantly metal-rich red clump (RC) stars. Unlike the RC stars, the RRL stars do not trace a strong bar, but have a more spheroidal, centrally concentrated distribution, showing only a slight elongation in its very center. We find a hint of bimodality in the density distribution at high southern latitudes (b < -5), which needs to be confirmed by extending the areal coverage of the current census. The different spatial distributions of the metal-rich and metal-poor stellar populations suggest that the Milky Way has a composite bulge. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1309.5933v1-abstract-full').style.display = 'none'; document.getElementById('1309.5933v1-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 September, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">Accepted for publication in The Astrophysical Journal Letters, copyright AAS 2013</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1307.0419">arXiv:1307.0419</a> <span> [<a href="https://arxiv.org/pdf/1307.0419">pdf</a>, <a href="https://arxiv.org/ps/1307.0419">ps</a>, <a href="https://arxiv.org/format/1307.0419">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"> Searching for variable stars in the VVV globular clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=D%C3%A9k%C3%A1ny%2C+I">Istv谩n D茅k谩ny</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=Ramos%2C+R+C">Rodrigo Contreras Ramos</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">Dante Minniti</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1307.0419v1-abstract-short" style="display: inline;"> The VVV is currently surveying the central regions of the Milky Way at near-infrared wavelengths, including 36 known Galactic globular clusters. We already have data in several filters to generate their color-magnitude diagrams. We also have enough epochs to begin producing the light-curves of the cluster stars and look for any possible member variable stars. We are especially interested in RR Lyr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1307.0419v1-abstract-full').style.display = 'inline'; document.getElementById('1307.0419v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1307.0419v1-abstract-full" style="display: none;"> The VVV is currently surveying the central regions of the Milky Way at near-infrared wavelengths, including 36 known Galactic globular clusters. We already have data in several filters to generate their color-magnitude diagrams. We also have enough epochs to begin producing the light-curves of the cluster stars and look for any possible member variable stars. We are especially interested in RR Lyrae stars, since they are abundant in Galactic globular clusters, and the period-luminosity relation they show at near-infrared wavelengths, can help enormously in providing accurate distances and reddenings for the most extincted and poorly studied inner Galactic globular clusters. We center our attention here in the preliminary analysis of three of these clusters: NGC 6441, Terzan 10 and 2MASS-GC02. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1307.0419v1-abstract-full').style.display = 'none'; document.getElementById('1307.0419v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 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">6 pages, 4 figures. To appear in the proceedings of "Fifty Years of Wide Field Studies in the Southern Hemisphere: Resolved Stellar Populations in the Galactic Bulge and the Magellanic Clouds", to be published in the Astronomical Society of the Pacific Conference Series</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1304.2673">arXiv:1304.2673</a> <span> [<a href="https://arxiv.org/pdf/1304.2673">pdf</a>, <a href="https://arxiv.org/ps/1304.2673">ps</a>, <a href="https://arxiv.org/format/1304.2673">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201321260">10.1051/0004-6361/201321260 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A near-infrared catalogue of the Galactic novae in the VVV survey area </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=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Angeloni%2C+R">R. Angeloni</a>, <a href="/search/astro-ph?searchtype=author&query=Catelan%2C+M">M. Catelan</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=Borissova%2C+J">J. Borissova</a>, <a href="/search/astro-ph?searchtype=author&query=Dekany%2C+I">I. Dekany</a>, <a href="/search/astro-ph?searchtype=author&query=Kerins%2C+E">E. Kerins</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtev%2C+R">R. Kurtev</a>, <a href="/search/astro-ph?searchtype=author&query=Mennickent%2C+R+E">R. E. Mennickent</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="1304.2673v1-abstract-short" style="display: inline;"> Near-IR data of Classical Novae contain useful information about the ejected gas mass and the thermal emission by dust formed during eruption, and provide independent methods to classify the objects according to the colour of their progenitors, and the fading rate and features seen after eruption. The VISTA Variables in the Via Lactea survey (VVV) is a near-IR ESO Public Survey mapping the MW bulg… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1304.2673v1-abstract-full').style.display = 'inline'; document.getElementById('1304.2673v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1304.2673v1-abstract-full" style="display: none;"> Near-IR data of Classical Novae contain useful information about the ejected gas mass and the thermal emission by dust formed during eruption, and provide independent methods to classify the objects according to the colour of their progenitors, and the fading rate and features seen after eruption. The VISTA Variables in the Via Lactea survey (VVV) is a near-IR ESO Public Survey mapping the MW bulge and southern plane. Data taken during 2010-2011 covered the entire area in the JHKs bands plus some epochs in Ks-band of the ongoing VVV variability campaign. We used the novae list provided by VSX/AAVSO catalogue to search for all objects within the VVV area. We used the VVV data to create a near-IR catalogue of the known Galactic novae in the 562 sq.deg. area covered by VVV. The VVV near-IR catalogue of novae contains JHKs photometry of 93 objects completed as of December 2012. We also checked in the ongoing VVV variability campaign for the light-curves of novae that erupted in the last years. VVV images can also be used to discover and study novae by searching for the expanding shell. Since objects are seen at different distances and reddening levels, the colour-magnitude and colour-colour diagrams show the novae spread in magnitude as well as in colour. Dereddened colours and reddening-free indices were used with caution and cannot be a good approach in all cases since the distance and spectral features prevent more conclusive results for some extreme objects. Light-curves for some recent novae are presented. Thanks to its high spatial resolution in the near-IR, and large Ks-range, the VVV survey can be a major contributor for the search and study of novae in the most crowded and high-extinction regions of the Milky Way. The VVV survey area contains ~35 of all known novae in the Galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1304.2673v1-abstract-full').style.display = 'none'; document.getElementById('1304.2673v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 April, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">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/1211.5291">arXiv:1211.5291</a> <span> [<a href="https://arxiv.org/pdf/1211.5291">pdf</a>, <a href="https://arxiv.org/ps/1211.5291">ps</a>, <a href="https://arxiv.org/format/1211.5291">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/sts473">10.1093/mnras/sts473 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Absolute parameters of AE For -- a highly active detached binary of late K type </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rozyczka%2C+M">M. Rozyczka</a>, <a href="/search/astro-ph?searchtype=author&query=Pietrukowicz%2C+P">P. Pietrukowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Kaluzny%2C+J">J. Kaluzny</a>, <a href="/search/astro-ph?searchtype=author&query=Pych%2C+W">W. Pych</a>, <a href="/search/astro-ph?searchtype=author&query=Angeloni%2C+R">R. Angeloni</a>, <a href="/search/astro-ph?searchtype=author&query=Dekany%2C+I">I. Dekany</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="1211.5291v1-abstract-short" style="display: inline;"> We present photometric and spectroscopic analysis of AE For -- a detached eclipsing binary composed of two late K dwarfs. The masses of the components are found to be 0.6314 +- 0.0035 and 0.6197 +- 0.0034 Msun and the radii to be 0.67 +- 0.03 and 0.63$ +- 0.03 Rsun for primary and secondary component, respectively. Both components are significantly oversized compared to theoretical models, which w… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1211.5291v1-abstract-full').style.display = 'inline'; document.getElementById('1211.5291v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1211.5291v1-abstract-full" style="display: none;"> We present photometric and spectroscopic analysis of AE For -- a detached eclipsing binary composed of two late K dwarfs. The masses of the components are found to be 0.6314 +- 0.0035 and 0.6197 +- 0.0034 Msun and the radii to be 0.67 +- 0.03 and 0.63$ +- 0.03 Rsun for primary and secondary component, respectively. Both components are significantly oversized compared to theoretical models, which we attribute to their high activity. They show Halpha, Hbeta, Hgamma, Ca H and Ca K lines in emission, and are heavily spotted, causing large variations of the light curve. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1211.5291v1-abstract-full').style.display = 'none'; document.getElementById('1211.5291v1-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 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">Accepted by 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/1112.3957">arXiv:1112.3957</a> <span> [<a href="https://arxiv.org/pdf/1112.3957">pdf</a>, <a href="https://arxiv.org/ps/1112.3957">ps</a>, <a href="https://arxiv.org/format/1112.3957">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201118614">10.1051/0004-6361/201118614 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Strengthening the Open Cluster Distance Scale via VVV Photometry </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Majaess%2C+D+J">Daniel J. Majaess</a>, <a href="/search/astro-ph?searchtype=author&query=Turner%2C+D+G">David G. Turner</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=Geisler%2C+D">D. Geisler</a>, <a href="/search/astro-ph?searchtype=author&query=Borissova%2C+J">J. Borissova</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Bonatto%2C+C">C. Bonatto</a>, <a href="/search/astro-ph?searchtype=author&query=Gieren%2C+W">W. Gieren</a>, <a href="/search/astro-ph?searchtype=author&query=Carraro%2C+G">G. Carraro</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtev%2C+R">R. Kurtev</a>, <a href="/search/astro-ph?searchtype=author&query=Mauro%2C+F">F. Mauro</a>, <a href="/search/astro-ph?searchtype=author&query=Chene%2C+A">A-N. Chene</a>, <a href="/search/astro-ph?searchtype=author&query=Forbes%2C+D+W">D. W. Forbes</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+P">P. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=Dekany%2C+I">I. Dekany</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=Soto%2C+M">M. Soto</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="1112.3957v1-abstract-short" style="display: inline;"> Approximately 14% of known Galactic open clusters possess absolute errors 20% as evaluated from n>3 independent distance estimates, and the statistics for age estimates are markedly worse. That impedes such diverse efforts as calibrating standard candles and constraining masses for substellar companions. New data from the VVV survey may be employed to establish precise cluster distances with compa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1112.3957v1-abstract-full').style.display = 'inline'; document.getElementById('1112.3957v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1112.3957v1-abstract-full" style="display: none;"> Approximately 14% of known Galactic open clusters possess absolute errors 20% as evaluated from n>3 independent distance estimates, and the statistics for age estimates are markedly worse. That impedes such diverse efforts as calibrating standard candles and constraining masses for substellar companions. New data from the VVV survey may be employed to establish precise cluster distances with comparatively reduced uncertainties (<10%). This is illustrated by deriving parameters for Pismis 19 and NGC 4349, two pertinent open clusters which hitherto feature sizable uncertainties (60%). Fundamental parameters determined for Pismis 19 from new VVV JHKs photometry are d=2.40+-0.15 kpc, <E(J-H)>=0.34+-0.04, and log(t)=9.05+-0.10, whereas for NGC 4349 the analysis yielded d=1.63+-0.13 kpc, E(J-H)=0.09+-0.02, log(t)=8.55+-0.10. The results exhibit a significant (>5x) reduction in uncertainties, and indicate that: i) existing parameters for the substellar object NGC 4349 127b require revision, in part because the new cluster parameters imply that the host is 20% less-massive (M*/Ms~3.1); ii) R Cru is not a member of NGC 4349 and should be excluded from period-Wesenheit calibrations that anchor the distance scale; iii) and results for Pismis 19 underscore the advantages gleaned from employing deep VVV JHKs data to examine obscured (Av~4) and differentially reddened intermediate-age clusters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1112.3957v1-abstract-full').style.display = 'none'; document.getElementById('1112.3957v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 December, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">To appear in A&A Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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/1111.0909">arXiv:1111.0909</a> <span> [<a href="https://arxiv.org/pdf/1111.0909">pdf</a>, <a href="https://arxiv.org/format/1111.0909">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The VISTA Variables in the Via Lactea survey: A first glance on stellar variability </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dekany%2C+I">I. Dekany</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=Collaboration%2C+t+V">the VVV Collaboration</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1111.0909v2-abstract-short" style="display: inline;"> VISTA Variables in the Via Lactea (VVV) is an ESO public near-infrared variability survey of the Galactic bulge and an adjacent area of the southern mid-plane. It will produce a deep atlas in the ZYJHKs filters, and a Ks-band time-series database of ~10^9 point sources, among which >~10^6 are expected to be variable. One of VVV's immediate scientific goals is to provide accurate light curves of pr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1111.0909v2-abstract-full').style.display = 'inline'; document.getElementById('1111.0909v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1111.0909v2-abstract-full" style="display: none;"> VISTA Variables in the Via Lactea (VVV) is an ESO public near-infrared variability survey of the Galactic bulge and an adjacent area of the southern mid-plane. It will produce a deep atlas in the ZYJHKs filters, and a Ks-band time-series database of ~10^9 point sources, among which >~10^6 are expected to be variable. One of VVV's immediate scientific goals is to provide accurate light curves of primary distance indicators, such as RR Lyrae stars, and utilize these data to produce a 3-D map of the surveyed area and, ultimately, trace the structure of the inner Galaxy. We give, based on the first ~1.5 years of the 5-yr-long survey, an early assessment on the basic properties and the overall quality of the VVV photometric time-series, and use these data to put an estimate of the fraction of variable stellar sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1111.0909v2-abstract-full').style.display = 'none'; document.getElementById('1111.0909v2-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 November, 2011; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 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">To appear in the proceedings of the Granada Stellar Pulsation conference, ed. L. A. Balona et al</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1110.0830">arXiv:1110.0830</a> <span> [<a href="https://arxiv.org/pdf/1110.0830">pdf</a>, <a href="https://arxiv.org/ps/1110.0830">ps</a>, <a href="https://arxiv.org/format/1110.0830">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/2041-8205/741/2/L27">10.1088/2041-8205/741/2/L27 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> New Evidence Supporting Membership for TW Nor in Lynga 6 and the Centaurus Spiral Arm </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Majaess%2C+D+J">Daniel J. Majaess</a>, <a href="/search/astro-ph?searchtype=author&query=Turner%2C+D+G">David G. Turner</a>, <a href="/search/astro-ph?searchtype=author&query=Bidin%2C+C+M">Christian Moni Bidin</a>, <a href="/search/astro-ph?searchtype=author&query=Mauro%2C+F">Francesco Mauro</a>, <a href="/search/astro-ph?searchtype=author&query=Geisler%2C+D">Douglas Geisler</a>, <a href="/search/astro-ph?searchtype=author&query=Gieren%2C+W">Wolfgang Gieren</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">Dante Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%C3%A9%2C+A">Andr茅-Nicolas Chen茅</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+P">Philip Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=Borissova%2C+J">Jura Borissova</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtev%2C+R">Radostn Kurtev</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%A9k%C3%A1ny%2C+I">Istvan D茅k谩ny</a>, <a href="/search/astro-ph?searchtype=author&query=Saito%2C+R+K">Roberto K. Saito</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="1110.0830v1-abstract-short" style="display: inline;"> The putative association between the 10.8 d classical Cepheid TW Nor and the open cluster Lynga 6 has generated considerable debate in the literature. New JHKs photometry in tandem with existing radial velocities for Lynga 6 stars imply cluster membership for TW Nor, and establish the variable as a high-weight calibrator for classical Cepheid relations. Fundamental mean parameters determined for L… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1110.0830v1-abstract-full').style.display = 'inline'; document.getElementById('1110.0830v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1110.0830v1-abstract-full" style="display: none;"> The putative association between the 10.8 d classical Cepheid TW Nor and the open cluster Lynga 6 has generated considerable debate in the literature. New JHKs photometry in tandem with existing radial velocities for Lynga 6 stars imply cluster membership for TW Nor, and establish the variable as a high-weight calibrator for classical Cepheid relations. Fundamental mean parameters determined for Lynga 6 are: d=1.91+-0.10 kpc, E(J-H)=0.38+-0.02, and log(t)=7.9+-0.1. The Benedict et al.(2007)/Turner (2010) Galactic VIc Wesenheit function was revised using TW Nor's new parameters: W_VI,0=(-3.37+-0.08)log(P_0)-2.48+-0.08. TW Nor/Lynga 6 lie beyond the Sagittarius-Carina spiral arm and occupy the Centaurus arm, along with innumerable young Cepheids and clusters (e.g., VW Cen & VVV CL070). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1110.0830v1-abstract-full').style.display = 'none'; document.getElementById('1110.0830v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 October, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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 (ApJ Letters)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1105.1119">arXiv:1105.1119</a> <span> [<a href="https://arxiv.org/pdf/1105.1119">pdf</a>, <a href="https://arxiv.org/format/1105.1119">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> The Vista Variables in the Via Lactea (VVV) ESO Public Survey: Current Status and First Results </p> <p class="authors"> <span class="search-hit">Authors:</span> <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+W">P. W. Lucas</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=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=Bonatto%2C+C">C. Bonatto</a>, <a href="/search/astro-ph?searchtype=author&query=Borissova%2C+J">J. Borissova</a>, <a href="/search/astro-ph?searchtype=author&query=Contreras%2C+C">C. Contreras</a>, <a href="/search/astro-ph?searchtype=author&query=Cross%2C+N">N. Cross</a>, <a href="/search/astro-ph?searchtype=author&query=Dekany%2C+I">I. Dekany</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=Eyheramendy%2C+S">S. Eyheramendy</a>, <a href="/search/astro-ph?searchtype=author&query=Geisler%2C+D">D. Geisler</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=Helminiak%2C+K+G">K. G. Helminiak</a>, <a href="/search/astro-ph?searchtype=author&query=Hempel%2C+M">M. Hempel</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=Ivanov%2C+V+D">V. D. Ivanov</a>, <a href="/search/astro-ph?searchtype=author&query=Jordan%2C+A">A. Jordan</a>, <a href="/search/astro-ph?searchtype=author&query=Kerins%2C+E">E. Kerins</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtev%2C+R">R. Kurtev</a>, <a href="/search/astro-ph?searchtype=author&query=Mauro%2C+F">F. Mauro</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=Navarrete%2C+C">C. Navarrete</a> , et al. (7 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1105.1119v2-abstract-short" style="display: inline;"> Vista Variables in the Via Lactea (VVV) is an ESO Public Survey that is performing a variability survey of the Galactic bulge and part of the inner disk using ESO's Visible and Infrared Survey Telescope for Astronomy (VISTA). The survey covers 520 deg^2 of sky area in the ZYJHK_S filters, for a total observing time of 1929 hours, including ~ 10^9 point sources and an estimated ~ 10^6 variable star… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1105.1119v2-abstract-full').style.display = 'inline'; document.getElementById('1105.1119v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1105.1119v2-abstract-full" style="display: none;"> Vista Variables in the Via Lactea (VVV) is an ESO Public Survey that is performing a variability survey of the Galactic bulge and part of the inner disk using ESO's Visible and Infrared Survey Telescope for Astronomy (VISTA). The survey covers 520 deg^2 of sky area in the ZYJHK_S filters, for a total observing time of 1929 hours, including ~ 10^9 point sources and an estimated ~ 10^6 variable stars. Here we describe the current status of the VVV Survey, in addition to a variety of new results based on VVV data, including light curves for variable stars, newly discovered globular clusters, open clusters, and associations. A set of reddening-free indices based on the ZYJHK_S system is also introduced. Finally, we provide an overview of the VVV Templates Project, whose main goal is to derive well-defined light curve templates in the near-IR, for the automated classification of VVV light curves. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1105.1119v2-abstract-full').style.display = 'none'; document.getElementById('1105.1119v2-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 June, 2011; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 May, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">25 pages, 18 figures. To appear in the Carnegie Observatories Astrophysics Series, Volume 5</span> </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Dekany%2C+I&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Dekany%2C+I&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Dekany%2C+I&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> </ul> </nav> <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 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