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<button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.20776">arXiv:2412.20776</a> <span> [<a href="https://arxiv.org/pdf/2412.20776">pdf</a>, <a href="https://arxiv.org/format/2412.20776">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/10.1051/0004-6361/202451517">10.1051/0004-6361/202451517 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Pristine survey. XXVI. Chemical abundances of subgiant stars of the extremelymetal-poor stream C-19 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bonifacio%2C+P">P. Bonifacio</a>, <a href="/search/astro-ph?searchtype=author&query=Caffau%2C+E">E. Caffau</a>, <a href="/search/astro-ph?searchtype=author&query=Fran%C3%A7ois%2C+P">P. Fran莽ois</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+N">N. Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Ibata%2C+R">R. Ibata</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+Z">Z. Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Kordopatis%2C+G">G. Kordopatis</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez%2C+J+I+G">J. I. Gonz谩lez Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Aguado%2C+D+S">D. S. Aguado</a>, <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+G+F">G. F. Thomas</a>, <a href="/search/astro-ph?searchtype=author&query=Viswanathan%2C+A">A. Viswanathan</a>, <a href="/search/astro-ph?searchtype=author&query=Dodd%2C+E">E. Dodd</a>, <a href="/search/astro-ph?searchtype=author&query=Gran%2C+F">F. Gran</a>, <a href="/search/astro-ph?searchtype=author&query=Starkenburg%2C+E">E. Starkenburg</a>, <a href="/search/astro-ph?searchtype=author&query=Lardo%2C+C">C. Lardo</a>, <a href="/search/astro-ph?searchtype=author&query=Errani%2C+R">R. Errani</a>, <a href="/search/astro-ph?searchtype=author&query=Fouesneau%2C+M">M. Fouesneau</a>, <a href="/search/astro-ph?searchtype=author&query=Navarro%2C+J+F">J. F. Navarro</a>, <a href="/search/astro-ph?searchtype=author&query=Venn%2C+K+A">K. A. Venn</a>, <a href="/search/astro-ph?searchtype=author&query=Malhan%2C+K">K. Malhan</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2412.20776v1-abstract-short" style="display: inline;"> Context: The C-19 stellar stream is the most metal-poor stream known to date. While its width and velocity dispersion indicate a dwarf galaxy origin, its metallicity spread and abundance patterns are more similar to those of globular clusters (GCs). If it is indeed of GC origin, its extremely low metallicity ([Fe/H]=-3.4, estimated from giant stars) implies that these stellar systems can form out… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.20776v1-abstract-full').style.display = 'inline'; document.getElementById('2412.20776v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.20776v1-abstract-full" style="display: none;"> Context: The C-19 stellar stream is the most metal-poor stream known to date. While its width and velocity dispersion indicate a dwarf galaxy origin, its metallicity spread and abundance patterns are more similar to those of globular clusters (GCs). If it is indeed of GC origin, its extremely low metallicity ([Fe/H]=-3.4, estimated from giant stars) implies that these stellar systems can form out of gas that is as extremely poor in metals as this. Previously, only giant stream stars were observed spectroscopically, although the majority of stream stars are unevolved stars. Aims: We pushed the spectroscopic observations to the subgiant branch stars ($G\approx 20$) in order to consolidate the chemical and dynamical properties of C-19. Methods: We used the high-efficiency spectrograph X-shooter fed by the ESO 8.2 m VLT telescope to observe 15 candidate subgiant C-19 members. The spectra were used to measure radial velocities and to determine chemical abundances using the \mygi\ code. Results; We developed a likelihood model that takes metallicity and radial velocities into account. We conclude that 12 stars are likely members of C-19, while 3 stars (S05, S12, and S13) are likely contaminants. When these 3 stars are excluded, our model implies a mean metallicity $\rm \langle [Fe/H]\rangle = -3.1\pm 0.1$, the mean radial velocity is $\langle v_r\rangle = -192\pm3$ kms$^{-1}$, and the velocity dispersion is $蟽_{vr} = 5.9^{+3.6}_{-5.9}$ kms$^{-1}$. This all agrees within errors with previous studies. The A(Mg) of a sample of 15 C-19 members, including 6 giant stars, shows a standard deviation of 0.44 dex, and the mean uncertainty on Mg is 0.25 dex. Conclusions: Our preferred interpretation of the current data is that C-19 is a disrupted GC. We cannot completely rule out the possibility that the GC could have belonged to a dwarf galaxy that contained more metal-rich stars, however. This scenario would explain the radial velocity members at higher metallicity, as well as the width and velocity dispersion of the stream. In either case, a GC formed out of gas as poor in metals as these stars seems necessary to explain the existence of C-19. The possibility that no GC was associated with C-19 cannot be ruled out either. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.20776v1-abstract-full').style.display = 'none'; document.getElementById('2412.20776v1-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Astronomy & Astrophysics - A&A, 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/2411.04623">arXiv:2411.04623</a> <span> [<a href="https://arxiv.org/pdf/2411.04623">pdf</a>, <a href="https://arxiv.org/format/2411.04623">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/10.1051/0004-6361/202452041">10.1051/0004-6361/202452041 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Unveiling VVV/WISE Mira variables on the far side of the Galactic disk: Distances, kinematics and a new extinction law </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Albarrac%C3%ADn%2C+R">Rogelio Albarrac铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Zoccali%2C+M">M. Zoccali</a>, <a href="/search/astro-ph?searchtype=author&query=Carvajal%2C+J+O">J. Olivares Carvajal</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas-Arriagada%2C+%C3%81">脕. Rojas-Arriagada</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+J+H">J. H. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Catelan%2C+M">M. Catelan</a>, <a href="/search/astro-ph?searchtype=author&query=De+Leo%2C+M">M. De Leo</a>, <a href="/search/astro-ph?searchtype=author&query=Gran%2C+F">F. Gran</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=Navarro%2C+%C3%81+V">脕. Valenzuela Navarro</a>, <a href="/search/astro-ph?searchtype=author&query=Salvo-Guajardo%2C+C">C. Salvo-Guajardo</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.04623v1-abstract-short" style="display: inline;"> The structure and kinematics of the Milky Way disk are largely inferred from the solar vicinity. To gain a comprehensive understanding, it is essential to find reliable tracers in less-explored regions like the bulge and the far side of the disk. Mira variables, which are well-studied and bright standard candles, offer an excellent opportunity to trace intermediate and old populations in these com… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.04623v1-abstract-full').style.display = 'inline'; document.getElementById('2411.04623v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.04623v1-abstract-full" style="display: none;"> The structure and kinematics of the Milky Way disk are largely inferred from the solar vicinity. To gain a comprehensive understanding, it is essential to find reliable tracers in less-explored regions like the bulge and the far side of the disk. Mira variables, which are well-studied and bright standard candles, offer an excellent opportunity to trace intermediate and old populations in these complex regions. We aim to isolate a clean sample of Miras in the Vista Variables in the V铆a L谩ctea survey using Gaussian process algorithms. This sample will be used to study intermediate and old age populations in the Galactic bulge and far disk. Near- and mid-infrared time-series photometry were processed using Gaussian Process algorithms to identify Mira variables and model their light curves. We calibrated selection criteria with a visually inspected sample to create a high-purity sample of Miras, integrating multi-band photometry and kinematic data from proper motions. We present a catalog of 3602 Mira variables. By analyzing photometry, we classify them by O-rich or C-rich surface chemistry and derive selective-to-total extinction ratios of $A_{K_{s}}/E(J - K_{s}) = 0.471 \pm 0.01$ and $A_{K_{s}}/E(H - K_{s}) = 1.320 \pm 0.020$. Using the Mira period-age relation, we find evidence supporting the inside-out formation of the Milky Way disk. The distribution of proper motions and distances aligns with the Galactic rotation curve and disk kinematics. We extend the rotation curve up to R$_{\rm GC} \sim 17 \ \rm{kpc}$ and find no strong evidence of the nuclear stellar disk in our Mira sample. This study constitutes the largest catalog of variable stars on the far side of the Galactic disk to date. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.04623v1-abstract-full').style.display = 'none'; document.getElementById('2411.04623v1-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 19 figures, Accepted 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 693, A28 (2025) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.11226">arXiv:2407.11226</a> <span> [<a href="https://arxiv.org/pdf/2407.11226">pdf</a>, <a href="https://arxiv.org/format/2407.11226">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/10.1051/0004-6361/202450126">10.1051/0004-6361/202450126 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> VVV catalog of ab-type RR Lyrae in the inner Galactic bulge </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zoccali%2C+M">M. Zoccali</a>, <a href="/search/astro-ph?searchtype=author&query=Quezada%2C+C">C. Quezada</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=Valenti%2C+E">E. Valenti</a>, <a href="/search/astro-ph?searchtype=author&query=Valenzuela-Navarro%2C+A">A. Valenzuela-Navarro</a>, <a href="/search/astro-ph?searchtype=author&query=Carvajal%2C+J+O">J. Olivares Carvajal</a>, <a href="/search/astro-ph?searchtype=author&query=Arriagada%2C+A+R">A. Rojas Arriagada</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+J+H">J. H. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Gran%2C+F">F. Gran</a>, <a href="/search/astro-ph?searchtype=author&query=De+Leo%2C+M">M. De Leo</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.11226v1-abstract-short" style="display: inline;"> Context. Observational evidence has accumulated in the past years, showing that the Galactic bulge includes two populations, a metal poor and a metal rich one that, in addition to a different metallicity, show different alpha over iron abundances, spatial distribution, and kinematics. While the metal rich, barred component has been fairly well characterized, the metal poor, spheroidal component ha… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.11226v1-abstract-full').style.display = 'inline'; document.getElementById('2407.11226v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.11226v1-abstract-full" style="display: none;"> Context. Observational evidence has accumulated in the past years, showing that the Galactic bulge includes two populations, a metal poor and a metal rich one that, in addition to a different metallicity, show different alpha over iron abundances, spatial distribution, and kinematics. While the metal rich, barred component has been fairly well characterized, the metal poor, spheroidal component has been more elusive and harder to describe. RR Lyrae variables are clean tracers of the old bulge component, and they are, on average, more metal poor than red clump stars. Aims. In the present paper, we provide a new catalog of 16488 ab type RR Lyrae variables in the bulge region within -10<l<10 and -2.8<b<2.8, extracted from multi epoch PSF photometry performed on VISTA Variable in the Via Lactea survey data. We used the catalog to constrain the shape of the old, metal poor, bulge stellar population. Methods. The identification of ab type RR Lyrae among a large sample of candidate variables of different types has been performed via a combination of a Random Forest classifier and visual inspection... [abridged] Results. We use the present catalog to derive the shape of their distribution around the Galactic Center, resulting in an elongated spheroid with projected axis ratio b/a~0.7 and inclination angle ~20 degrees. We discuss how observational biases such as errors on the distances and a non-uniform sampling in longitude, affect both the present measurements and previous ones, especially those based on red clump stars... [abridged] Conclusions. We publish a high purity RRab sample for future studies of the oldest Galactic bulge population, close to the midplane. We explore different choices for the period-luminosity-metallicity relation, highlighting how some of them introduce spurious trends of distances with either period or metallicity, or both... [abridged] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.11226v1-abstract-full').style.display = 'none'; document.getElementById('2407.11226v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 689, A240 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.16646">arXiv:2406.16646</a> <span> [<a href="https://arxiv.org/pdf/2406.16646">pdf</a>, <a href="https://arxiv.org/format/2406.16646">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202450584">10.1051/0004-6361/202450584 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The VISTA Variables in the V铆a L谩ctea eXtended (VVVX) ESO public survey: Completion of the observations and legacy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Saito%2C+R+K">R. K. Saito</a>, <a href="/search/astro-ph?searchtype=author&query=Hempel%2C+M">M. Hempel</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso-Garc%C3%ADa%2C+J">J. Alonso-Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+P+W">P. W. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso%2C+S">S. Alonso</a>, <a href="/search/astro-ph?searchtype=author&query=Baravalle%2C+L">L. Baravalle</a>, <a href="/search/astro-ph?searchtype=author&query=Borissova%2C+J">J. Borissova</a>, <a href="/search/astro-ph?searchtype=author&query=Caceres%2C+C">C. Caceres</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%C3%A9%2C+A+N">A. N. Chen茅</a>, <a href="/search/astro-ph?searchtype=author&query=Cross%2C+N+J+G">N. J. G. Cross</a>, <a href="/search/astro-ph?searchtype=author&query=Duplancic%2C+F">F. Duplancic</a>, <a href="/search/astro-ph?searchtype=author&query=Garro%2C+E+R">E. R. Garro</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%B3mez%2C+M">M. G贸mez</a>, <a href="/search/astro-ph?searchtype=author&query=Ivanov%2C+V+D">V. D. Ivanov</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtev%2C+R">R. Kurtev</a>, <a href="/search/astro-ph?searchtype=author&query=Luna%2C+A">A. Luna</a>, <a href="/search/astro-ph?searchtype=author&query=Majaess%2C+D">D. Majaess</a>, <a href="/search/astro-ph?searchtype=author&query=Navarro%2C+M+G">M. G. Navarro</a>, <a href="/search/astro-ph?searchtype=author&query=Pullen%2C+J+B">J. B. Pullen</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">M. Rejkuba</a>, <a href="/search/astro-ph?searchtype=author&query=Sanders%2C+J+L">J. L. Sanders</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+L+C">L. C. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Albino%2C+P+H+C">P. H. C. Albino</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso%2C+M+V">M. V. Alonso</a> , et al. (121 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.16646v1-abstract-short" style="display: inline;"> The ESO public survey VISTA Variables in the V铆a L谩ctea (VVV) surveyed the inner Galactic bulge and the adjacent southern Galactic disk from $2009-2015$. Upon its conclusion, the complementary VVV eXtended (VVVX) survey has expanded both the temporal as well as spatial coverage of the original VVV area, widening it from $562$ to $1700$ sq. deg., as well as providing additional epochs in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.16646v1-abstract-full').style.display = 'inline'; document.getElementById('2406.16646v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.16646v1-abstract-full" style="display: none;"> The ESO public survey VISTA Variables in the V铆a L谩ctea (VVV) surveyed the inner Galactic bulge and the adjacent southern Galactic disk from $2009-2015$. Upon its conclusion, the complementary VVV eXtended (VVVX) survey has expanded both the temporal as well as spatial coverage of the original VVV area, widening it from $562$ to $1700$ sq. deg., as well as providing additional epochs in $JHK_{\rm s}$ filters from $2016-2023$. With the completion of VVVX observations during the first semester of 2023, we present here the observing strategy, a description of data quality and access, and the legacy of VVVX. VVVX took $\sim 2000$ hours, covering about 4% of the sky in the bulge and southern disk. VVVX covered most of the gaps left between the VVV and the VISTA Hemisphere Survey (VHS) areas and extended the VVV time baseline in the obscured regions affected by high extinction and hence hidden from optical observations. VVVX provides a deep $JHK_{\rm s}$ catalogue of $\gtrsim 1.5\times10^9$ point sources, as well as a $K_{\rm s}$ band catalogue of $\sim 10^7$ variable sources. Within the existing VVV area, we produced a $5D$ map of the surveyed region by combining positions, distances, and proper motions of well-understood distance indicators such as red clump stars, RR Lyrae, and Cepheid variables. In March 2023 we successfully finished the VVVX survey observations that started in 2016, an accomplishment for ESO Paranal Observatory upon 4200 hours of observations for VVV+VVVX. The VVV+VVVX catalogues complement those from the Gaia mission at low Galactic latitudes and provide spectroscopic targets for the forthcoming ESO high-multiplex spectrographs MOONS and 4MOST. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.16646v1-abstract-full').style.display = 'none'; document.getElementById('2406.16646v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 11 figures (+ appendix). Accepted for publication in Astronomy and Astrophysics in section 14: Catalogs and data</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 689, A148 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.05728">arXiv:2406.05728</a> <span> [<a href="https://arxiv.org/pdf/2406.05728">pdf</a>, <a href="https://arxiv.org/format/2406.05728">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The Pristine survey XXIV: The Galactic underdogs -- Dynamic tales of a Milky Way metal-poor population </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=de+La+Vernhe%2C+I+G+R">Isaure Gonz谩lez Rivera de La Vernhe</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+V">Vanessa Hill</a>, <a href="/search/astro-ph?searchtype=author&query=Kordopatis%2C+G">Georges Kordopatis</a>, <a href="/search/astro-ph?searchtype=author&query=Gran%2C+F">Felipe Gran</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez-Alvar%2C+E">Emma Fern谩ndez-Alvar</a>, <a href="/search/astro-ph?searchtype=author&query=Ardern-Arentsen%2C+A">Anke Ardern-Arentsen</a>, <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+G+F">Guillaume F. Thomas</a>, <a href="/search/astro-ph?searchtype=author&query=Sestito%2C+F">Federico Sestito</a>, <a href="/search/astro-ph?searchtype=author&query=Navarrete%2C+C">Camila Navarrete</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+N+F">Nicolas F. Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Starkenburg%2C+E">Else Starkenburg</a>, <a href="/search/astro-ph?searchtype=author&query=Viswanathan%2C+A">Akshara Viswanathan</a>, <a href="/search/astro-ph?searchtype=author&query=Battaglia%2C+G">Giuseppina Battaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Venn%2C+K+A">Kim A. Venn</a>, <a href="/search/astro-ph?searchtype=author&query=Vitali%2C+S">Sara Vitali</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.05728v3-abstract-short" style="display: inline;"> Through the chemodynamical characterisation of metal-poor stars, one can efficiently probe the early history of the Milky Way. We aim at decontaminating a sample of $\sim$ 3M giant stars with Gaia DR3 XP-based \textit{Pristine-Gaia} metallicities, to investigate a subset of very metal-poor stars ([Fe/H] < -1.7) with disc-like orbits. We construct a statistically robust sample of $\sim$ 36 000 very… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.05728v3-abstract-full').style.display = 'inline'; document.getElementById('2406.05728v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.05728v3-abstract-full" style="display: none;"> Through the chemodynamical characterisation of metal-poor stars, one can efficiently probe the early history of the Milky Way. We aim at decontaminating a sample of $\sim$ 3M giant stars with Gaia DR3 XP-based \textit{Pristine-Gaia} metallicities, to investigate a subset of very metal-poor stars ([Fe/H] < -1.7) with disc-like orbits. We construct a statistically robust sample of $\sim$ 36 000 very metal-poor giants, using APOGEE and LAMOST to estimate and remove contamination from high $V_蠁$ stars. We investigate the spatial and kinematic properties of the decontaminated sample, using $V_蠁$ and the action space, both powerful to disentangle stellar populations. As in previous works, we find a pronounced asymmetry in $L_z$ and $V_蠁$ in favour of prograde stars. This excess is mostly made of prograde-planar stars (10% of the very metal-poor population), and contains stars with $V_蠁$ > 180 km s$^{-1}$ and $Z_{\text{max}}$ < 1.5 kpc, down to [Fe/H] = -2.9 at a 2$蟽$ confidence level. While the overall orbital distributions of our sample match that of a halo, the highly prograde and planar subset (2% of the very metal-poor population) also bears characteristics classically associated with a thick disc, i.e., a spatial distribution compatible with a short-scaled thick disc, and a thick disc-like $Z_{\text{max}}$ - $R_{\text{max}}$ distribution. Additionally, assuming a stationary or prograde halo with $\overline{V_蠁}$ $\sim$ 30-40 km.s$^{-1}$ is not sufficient to suppress the kinematic signature of the highly prograde and planar subset. These results rule out any link with a thin disc, and instead, support a contribution from a \textit{metal-weak thick disc}. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.05728v3-abstract-full').style.display = 'none'; document.getElementById('2406.05728v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A on June 24, 2024. The abstract has been modified to comply with arXiv's abstract requirements (word limit). The paper numbering has been modified from XXV to XXIV to remain consistent with the recent submissions of the Pristine collaboration</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.13124">arXiv:2405.13124</a> <span> [<a href="https://arxiv.org/pdf/2405.13124">pdf</a>, <a href="https://arxiv.org/format/2405.13124">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 Pristine survey -- XXVI. The very metal-poor Galaxy: Chemodynamics through the follow-up of the Pristine-Gaia synthetic catalogue </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Viswanathan%2C+A">Akshara Viswanathan</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+Z">Zhen Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Ardern-Arentsen%2C+A">Anke Ardern-Arentsen</a>, <a href="/search/astro-ph?searchtype=author&query=Starkenburg%2C+E">Else Starkenburg</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+N+F">Nicolas F. Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Youakim%2C+K">Kris Youakim</a>, <a href="/search/astro-ph?searchtype=author&query=Ibata%2C+R+A">Rodrigo A. Ibata</a>, <a href="/search/astro-ph?searchtype=author&query=Sestito%2C+F">Federico Sestito</a>, <a href="/search/astro-ph?searchtype=author&query=Matsuno%2C+T">Tadafumi Matsuno</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+C+A">Carlos Allende Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Barwell%2C+F">Freya Barwell</a>, <a href="/search/astro-ph?searchtype=author&query=Bayer%2C+M">Manuel Bayer</a>, <a href="/search/astro-ph?searchtype=author&query=Doliva-Dolinsky%2C+A">Amandine Doliva-Dolinsky</a>, <a href="/search/astro-ph?searchtype=author&query=Fernandez-Alvar%2C+E">Emma Fernandez-Alvar</a>, <a href="/search/astro-ph?searchtype=author&query=Anta%2C+P+M+G">Pablo M. Galan-de Anta</a>, <a href="/search/astro-ph?searchtype=author&query=Jhass%2C+K">Kiran Jhass</a>, <a href="/search/astro-ph?searchtype=author&query=Longeard%2C+N">Nicolas Longeard</a>, <a href="/search/astro-ph?searchtype=author&query=Arroyo-Polonio%2C+J+M">Jose Maria Arroyo-Polonio</a>, <a href="/search/astro-ph?searchtype=author&query=Massana%2C+P">Pol Massana</a>, <a href="/search/astro-ph?searchtype=author&query=Montelius%2C+M">Martin Montelius</a>, <a href="/search/astro-ph?searchtype=author&query=Rusterucci%2C+S">Samuel Rusterucci</a>, <a href="/search/astro-ph?searchtype=author&query=Santos%2C+J">Judith Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+G+F">Guillaume F. Thomas</a>, <a href="/search/astro-ph?searchtype=author&query=Vitali%2C+S">Sara Vitali</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+W">Wenbo Wu</a> , et al. (5 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.13124v1-abstract-short" style="display: inline;"> The Pristine-\textit{Gaia} synthetic catalogue provides reliable photometric metallicities for $\sim$30 million FGK stars using the Pristine survey model and Gaia XP spectra. We perform the first low-to-medium-resolution spectroscopic follow-up of bright (G<15) and distant (up to 35 kpc) very and extremely metal-poor (V/EMP, [Fe/H]<-2.5) red giant branch stars from this. We use Isaac Newton Telesc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13124v1-abstract-full').style.display = 'inline'; document.getElementById('2405.13124v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.13124v1-abstract-full" style="display: none;"> The Pristine-\textit{Gaia} synthetic catalogue provides reliable photometric metallicities for $\sim$30 million FGK stars using the Pristine survey model and Gaia XP spectra. We perform the first low-to-medium-resolution spectroscopic follow-up of bright (G<15) and distant (up to 35 kpc) very and extremely metal-poor (V/EMP, [Fe/H]<-2.5) red giant branch stars from this. We use Isaac Newton Telescope/Intermediate Dispersion Spectrograph (INT/IDS) observations centred around the calcium triplet region ideal for V/EMP stars. We find that 76\% of our stars indeed have [Fe/H]<-2.5 with these inferred spectroscopic metallicities and only 3\% are outliers with [Fe/H] > -2.0. We report a success rate of 77\% and 38\% in finding stars with [Fe/H]<-2.5 and -3.0 respectively. This will allow for 10,000-20,000 homogeneously analysed EMP stars using the WEAVE survey follow-up of Pristine EMP candidates. We associate 20\%, 46\%, and 34\% of the stars to be confined to the disc plane, or to have inner and outer halo orbits, respectively. We also associate these V/EMP stars to known accretion events such as Gaia-Enceladus-Sausage (GES), LMS-1/Wukong, Thamnos, Helmi streams, Sagittarius, Sequoia, etc. For the stars that orbit close to the disc plane, we find that the prograde region with low vertical action is overdense with a significance of 4$蟽$ as compared to its retrograde counterpart. We also find three new (brightest) members of the most metal-poor stellar stream, C-19, one of which is 50$^\circ$ away from the main body of the stream. Our measured mean metallicity, velocity dispersion, and stream width are consistent with the literature, but our results favour a higher distance ($\sim$21.5 kpc) for the stream. We publish a catalogue (and 1D spectra) of 215 V/EMP stars from this spectroscopic follow-up and showcase the power of chemokinematic analysis of V/EMP end. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13124v1-abstract-full').style.display = 'none'; document.getElementById('2405.13124v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to A&A. 17 pages (9 figures) + 3 pages (3 figures) in Appendix. Comments are very welcome! The catalogue and 1D spectra will be made available public after acceptance and before upon reasonable request to the first author</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.00096">arXiv:2405.00096</a> <span> [<a href="https://arxiv.org/pdf/2405.00096">pdf</a>, <a href="https://arxiv.org/format/2405.00096">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/10.1051/0004-6361/202450553">10.1051/0004-6361/202450553 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Pristine Inner Galaxy Survey (PIGS) IX. The largest detailed chemical analysis of very metal-poor stars in the Sagittarius dwarf galaxy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sestito%2C+F">Federico Sestito</a>, <a href="/search/astro-ph?searchtype=author&query=Vitali%2C+S">Sara Vitali</a>, <a href="/search/astro-ph?searchtype=author&query=Jofre%2C+P">Paula Jofre</a>, <a href="/search/astro-ph?searchtype=author&query=Venn%2C+K+A">Kim A. Venn</a>, <a href="/search/astro-ph?searchtype=author&query=Aguado%2C+D+S">David S. Aguado</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilera-G%C3%B3mez%2C+C">Claudia Aguilera-G贸mez</a>, <a href="/search/astro-ph?searchtype=author&query=Ardern-Arentsen%2C+A">Anke Ardern-Arentsen</a>, <a href="/search/astro-ph?searchtype=author&query=Silva%2C+D+d+B">Danielle de Brito Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Carlberg%2C+R">Raymond Carlberg</a>, <a href="/search/astro-ph?searchtype=author&query=Eldridge%2C+C+J+L">Camilla J. L. Eldridge</a>, <a href="/search/astro-ph?searchtype=author&query=Gran%2C+F">Felipe Gran</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+V">Vanessa Hill</a>, <a href="/search/astro-ph?searchtype=author&query=Jablonka%2C+P">Pascale Jablonka</a>, <a href="/search/astro-ph?searchtype=author&query=Kordopatis%2C+G">Georges Kordopatis</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+N+F">Nicolas F. Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Matsuno%2C+T">Tadafumi Matsuno</a>, <a href="/search/astro-ph?searchtype=author&query=Rusterucci%2C+S">Samuel Rusterucci</a>, <a href="/search/astro-ph?searchtype=author&query=Starkenburg%2C+E">Else Starkenburg</a>, <a href="/search/astro-ph?searchtype=author&query=Viswanathan%2C+A">Akshara Viswanathan</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.00096v2-abstract-short" style="display: inline;"> The most metal-poor stars provide valuable insights into the early chemical enrichment history of a system, carrying the chemical imprints of the first generations of supernovae. The most metal-poor region of the Sagittarius dwarf galaxy remains inadequately observed and characterised. To date, only $\sim4$ stars with [Fe/H]~$<-2.0$ have been chemically analysed with high-resolution spectroscopy.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.00096v2-abstract-full').style.display = 'inline'; document.getElementById('2405.00096v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.00096v2-abstract-full" style="display: none;"> The most metal-poor stars provide valuable insights into the early chemical enrichment history of a system, carrying the chemical imprints of the first generations of supernovae. The most metal-poor region of the Sagittarius dwarf galaxy remains inadequately observed and characterised. To date, only $\sim4$ stars with [Fe/H]~$<-2.0$ have been chemically analysed with high-resolution spectroscopy. In this study, we present the most extensive chemical abundance analysis of 12 low-metallicity stars with metallicities down to [Fe/H]~$=-3.26$ and located in the main body of Sagittarius. These targets, selected from the Pristine Inner Galaxy Survey, were observed using the MIKE high-resolution spectrograph at the {\it Magellan-Clay} telescope, which allowed us to measure up to 17 chemical species. The chemical composition of these stars reflects the imprint of a variety of type~II supernovae (SNe~II). A combination of low- to intermediate-mass high-energy SNe and hypernovae ($\sim10-70\msun$) is required to account for the abundance patterns of the lighter elements up to the Fe-peak. The trend of the heavy elements suggests the involvement of compact binary merger events and fast-rotating (up to $\sim300\kms$) intermediate-mass to massive metal-poor stars ($\sim25-120\msun$) that are the sources of rapid and slow processes, respectively. Additionally, asymptotic giant branch stars contribute to a wide dispersion of [Ba/Mg] and [Ba/Eu]. The absence of an $伪-$knee in our data indicates that type Ia supernovae did not contribute in the very metal-poor region ([Fe/H]~$\leq-2.0$). However, they might have started to pollute the interstellar medium at [Fe/H]~$>-2.0$, given the relatively low [Co/Fe] in this metallicity region. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.00096v2-abstract-full').style.display = 'none'; document.getElementById('2405.00096v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A. New plot on [Eu/Mg]. Some refs updated</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 689, A201 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.02578">arXiv:2404.02578</a> <span> [<a href="https://arxiv.org/pdf/2404.02578">pdf</a>, <a href="https://arxiv.org/format/2404.02578">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/10.1051/0004-6361/202450198">10.1051/0004-6361/202450198 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> SpectroTranslator: a deep-neural network algorithm to homogenize spectroscopic parameters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+G+F">G. F. Thomas</a>, <a href="/search/astro-ph?searchtype=author&query=Battaglia%2C+G">G. Battaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Gran%2C+F">F. Gran</a>, <a href="/search/astro-ph?searchtype=author&query=Fernandez-Alvar%2C+E">E. Fernandez-Alvar</a>, <a href="/search/astro-ph?searchtype=author&query=Tsantaki%2C+M">M. Tsantaki</a>, <a href="/search/astro-ph?searchtype=author&query=Pancino%2C+E">E. Pancino</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+V">V. Hill</a>, <a href="/search/astro-ph?searchtype=author&query=Kordopatis%2C+G">G. Kordopatis</a>, <a href="/search/astro-ph?searchtype=author&query=Gallart%2C+C">C. Gallart</a>, <a href="/search/astro-ph?searchtype=author&query=Turchi%2C+A">A. Turchi</a>, <a href="/search/astro-ph?searchtype=author&query=Masseron%2C+T">T. Masseron</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="2404.02578v1-abstract-short" style="display: inline;"> The emergence of large spectroscopic surveys requires homogenising on the same scale the quantities they measure in order to increase their scientific legacy. We developed the SpectroTranslator, a data-driven deep neural network algorithm that can convert spectroscopic parameters from the base of one survey to another. The algorithm also includes a method to estimate the importance that the variou… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.02578v1-abstract-full').style.display = 'inline'; document.getElementById('2404.02578v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.02578v1-abstract-full" style="display: none;"> The emergence of large spectroscopic surveys requires homogenising on the same scale the quantities they measure in order to increase their scientific legacy. We developed the SpectroTranslator, a data-driven deep neural network algorithm that can convert spectroscopic parameters from the base of one survey to another. The algorithm also includes a method to estimate the importance that the various parameters play in the conversion from base A to B. As a showcase, we apply the algorithm to transform effective temperature, surface gravity, metallicity, [Mg/Fe] and los velocity from the base of GALAH into the APOGEE base. We demonstrate the efficiency of the SpectroTranslator algorithm to translate the spectroscopic parameters from one base to another using parameters directly by the survey teams, and are able to achieve a similar performance than previous works that have performed a similar type of conversion but using the full spectrum rather than the spectroscopic parameters, allowing to reduce the computational time, and to use the output of pipelines optimized for each survey. By combining the transformed GALAH catalogue with the APOGEE catalogue, we study the distribution of [Fe/H] and [Mg/Fe] across the Galaxy, and we find that the median distribution of both quantities present a vertical asymmetry at large radii. We attribute it to the recent perturbations generated by the passage of a dwarf galaxy across the disc or by the infall of the Large Magellanic Cloud. Although several aspects still need to be refined, in particular how to deal in an optimal manner with regions of the parameter space meagrely populated by stars in the training sample, the SpectroTranslator already shows its capability and promises to play a crucial role in standardizing various spectroscopic surveys onto a unified basis. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.02578v1-abstract-full').style.display = 'none'; document.getElementById('2404.02578v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 April, 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">27 pages. Submitted to A&A. Webpage related to the paper: https://research.iac.es/proyecto/spectrotranslator/</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 690, A54 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.09868">arXiv:2310.09868</a> <span> [<a href="https://arxiv.org/pdf/2310.09868">pdf</a>, <a href="https://arxiv.org/format/2310.09868">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 treasure behind the haystack: MUSE analysis of five recently discovered globular clusters </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=Kordopatis%2C+G">G. Kordopatis</a>, <a href="/search/astro-ph?searchtype=author&query=Zoccali%2C+M">M. Zoccali</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+V">V. Hill</a>, <a href="/search/astro-ph?searchtype=author&query=Saviane%2C+I">I. Saviane</a>, <a href="/search/astro-ph?searchtype=author&query=Navarrete%2C+C">C. Navarrete</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas-Arriagada%2C+A">A. Rojas-Arriagada</a>, <a href="/search/astro-ph?searchtype=author&query=Carballo-Bello%2C+J">J. Carballo-Bello</a>, <a href="/search/astro-ph?searchtype=author&query=Hartke%2C+J">J. Hartke</a>, <a href="/search/astro-ph?searchtype=author&query=Valenti%2C+E">E. Valenti</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=De+Leo%2C+M">M. De Leo</a>, <a href="/search/astro-ph?searchtype=author&query=Fabbro%2C+S">S. Fabbro</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="2310.09868v1-abstract-short" style="display: inline;"> After the second data release of Gaia, the number of new globular cluster candidates has increased importantly. However, most of them need to be properly characterised, both spectroscopically and photometrically, by means of radial velocities, metallicities, and deeper photometric observations. Our goal is to provide an independent confirmation of the cluster nature of Gran 4, a recently discovere… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.09868v1-abstract-full').style.display = 'inline'; document.getElementById('2310.09868v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.09868v1-abstract-full" style="display: none;"> After the second data release of Gaia, the number of new globular cluster candidates has increased importantly. However, most of them need to be properly characterised, both spectroscopically and photometrically, by means of radial velocities, metallicities, and deeper photometric observations. Our goal is to provide an independent confirmation of the cluster nature of Gran 4, a recently discovered globular cluster, with follow-up spectroscopic observations. The derived radial velocity for individual stars, coupled with proper motions, allows us to isolate cluster members from field stars, while the analysis of their spectra allows us to derive metallicities. By including in the analysis the recently confirmed clusters Gran 1, 2, 3, and 5, we aim to completely characterise the sample presented in Gran et al. 2022. Using Gaia DR3 and VVV catalogue data and MUSE@VLT observations, we performed a selection of cluster members based on their proper motions, radial velocities and their position in colour-magnitude diagrams. Furthermore, full spectral synthesis was performed on the cluster members, extracting surface parameters and metallicity from MUSE spectra. Finally, a completeness estimation was performed on the total globular cluster population of the Milky Way. We confirm the nature of Gran 4, a newly discovered globular cluster behind the Galactic bulge, with a mean radial velocity of ${\rm RV} = -265.28 \pm 3.92$ km s$^{-1}$ and a mean metallicity of ${\rm [Fe/H] = -1.72 \pm 0.32}$ dex. Additionally, independent measurements of the metallicities were derived for Gran 1, 2, 3, and 5. We also revise the observational lower mass limit for a globular cluster to survive in the bulge/disk environment. We estimate that $\sim 12-26$ globular clusters have still to be discovered on the other side of the Galaxy (i.e., behind the bulge/bar/disk), up to 20 kpc. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.09868v1-abstract-full').style.display = 'none'; document.getElementById('2310.09868v1-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 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">8 pages, 5 figures, appendix: 5 tables and 1 figure. Accepted for publication for 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/2308.01344">arXiv:2308.01344</a> <span> [<a href="https://arxiv.org/pdf/2308.01344">pdf</a>, <a href="https://arxiv.org/format/2308.01344">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/10.1051/0004-6361/202347633">10.1051/0004-6361/202347633 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Pristine survey -- XXIII. Data Release 1 and an all-sky metallicity catalogue based on Gaia DR3 BP/RP spectro-photometry </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Martin%2C+N+F">Nicolas F. Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Starkenburg%2C+E">Else Starkenburg</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+Z">Zhen Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Fouesneau%2C+M">Morgan Fouesneau</a>, <a href="/search/astro-ph?searchtype=author&query=Ardern-Arentsen%2C+A">Anke Ardern-Arentsen</a>, <a href="/search/astro-ph?searchtype=author&query=De+Angeli%2C+F">Francesca De Angeli</a>, <a href="/search/astro-ph?searchtype=author&query=Gran%2C+F">Felipe Gran</a>, <a href="/search/astro-ph?searchtype=author&query=Montelius%2C+M">Martin Montelius</a>, <a href="/search/astro-ph?searchtype=author&query=Rusterucci%2C+S">Samuel Rusterucci</a>, <a href="/search/astro-ph?searchtype=author&query=Andrae%2C+R">Ren茅 Andrae</a>, <a href="/search/astro-ph?searchtype=author&query=Bellazzini%2C+M">Michele Bellazzini</a>, <a href="/search/astro-ph?searchtype=author&query=Montegriffo%2C+P">Paolo Montegriffo</a>, <a href="/search/astro-ph?searchtype=author&query=Esselink%2C+A+F">Anna F. Esselink</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+H">Hanyuan Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Venn%2C+K+A">Kim A. Venn</a>, <a href="/search/astro-ph?searchtype=author&query=Viswanathan%2C+A">Akshara Viswanathan</a>, <a href="/search/astro-ph?searchtype=author&query=Aguado%2C+D+S">David S. Aguado</a>, <a href="/search/astro-ph?searchtype=author&query=Battaglia%2C+G">Giuseppina Battaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Bayer%2C+M">Manuel Bayer</a>, <a href="/search/astro-ph?searchtype=author&query=Bonifacio%2C+P">Piercarlo Bonifacio</a>, <a href="/search/astro-ph?searchtype=author&query=Caffau%2C+E">Elisabetta Caffau</a>, <a href="/search/astro-ph?searchtype=author&query=C%C3%B4t%C3%A9%2C+P">Patrick C么t茅</a>, <a href="/search/astro-ph?searchtype=author&query=Carlberg%2C+R">Raymond Carlberg</a>, <a href="/search/astro-ph?searchtype=author&query=Fabbro%2C+S">S茅bastien Fabbro</a>, <a href="/search/astro-ph?searchtype=author&query=Alvar%2C+E+F">Emma Fern谩ndez Alvar</a> , et al. (16 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="2308.01344v2-abstract-short" style="display: inline;"> We used the spectro-photometric information of ~219 million stars from Gaia's DR3 to calculate synthetic, narrow-band, metallicity-sensitive CaHK magnitudes that mimic the observations of the Pristine survey, a survey of photometric metallicities of Milky Way (MW) stars that has been mapping >6,500 deg^2 of the northern sky with CFHT since 2015. These synthetic magnitudes were used for an absolute… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.01344v2-abstract-full').style.display = 'inline'; document.getElementById('2308.01344v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.01344v2-abstract-full" style="display: none;"> We used the spectro-photometric information of ~219 million stars from Gaia's DR3 to calculate synthetic, narrow-band, metallicity-sensitive CaHK magnitudes that mimic the observations of the Pristine survey, a survey of photometric metallicities of Milky Way (MW) stars that has been mapping >6,500 deg^2 of the northern sky with CFHT since 2015. These synthetic magnitudes were used for an absolute recalibration of the deeper Pristine photometry and, combined with broadband Gaia information, synthetic and Pristine CaHK magnitudes were used to estimate photometric metallicities over the whole sky. The resulting metallicity catalogue is accurate down to [Fe/H]~-3.5 and is particularly suited for the exploration of the metal-poor MW ([Fe/H]<-1.0). We make available here the catalogue of synthetic CaHK_syn magnitudes for all stars with BP/RP information in Gaia DR3, as well as an associated catalogue of more than ~30 million photometric metallicities for high S/N FGK stars. This paper further provides the first public data release of the Pristine catalogue in the form of higher quality recalibrated Pristine CaHK magnitudes and photometric metallicities for all stars in common with the BP/RP spectro-photometric information in Gaia DR3. When available, the much deeper Pristine data greatly enhance the quality of the derived metallicities, in particular at the faint end of the catalogue (G_BP > 16). Combined, both photometric metallicity catalogues include more than two million metal-poor star candidates ([Fe/H]_phot<-1.0) as well as more than 200,000 and ~8,000 very and extremely metal-poor candidates ([Fe/H]_phot<-2.0 and <-3.0, respectively). Finally, we show that these metallicity catalogues can be used efficiently, among other applications to hunt for the most metal-poor stars, and to study how the structure of the MW varies with metallicity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.01344v2-abstract-full').style.display = 'none'; document.getElementById('2308.01344v2-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">31 pages, 25 figures, accepted for publication in A&A. Minor changes in v2, including ~2.5% more coverage for Pristine DR1 from new observations. First two authors are co-first author. The CaHK photometry catalogue and the two photometric metallicity catalogues are available, before acceptance, as large compressed csv files at: https://seafile.unistra.fr/d/ee0c0f05719d4368bcbb/</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 692, A115 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.06628">arXiv:2204.06628</a> <span> [<a href="https://arxiv.org/pdf/2204.06628">pdf</a>, <a href="https://arxiv.org/format/2204.06628">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/stac934">10.1093/mnras/stac934 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Spectroscopic analysis of VVV CL001 cluster with MUSE </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Carvajal%2C+J+O">Julio Olivares Carvajal</a>, <a href="/search/astro-ph?searchtype=author&query=Zoccali%2C+M">Manuela Zoccali</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas-Arriagada%2C+A">Alvaro Rojas-Arriagada</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=Valenti%2C+E">Elena Valenti</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+J+H">Javier H. 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="2204.06628v1-abstract-short" style="display: inline;"> Like most spiral galaxies, the Milky Way contains a population of blue, metal-poor globular clusters and another of red, metal-rich ones. Most of the latter belong to the bulge, and therefore they are poorly studied compared to the blue (halo) ones because they suffer higher extinction and larger contamination from field stars. These intrinsic difficulties, together with a lack of low-mass bulge g… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.06628v1-abstract-full').style.display = 'inline'; document.getElementById('2204.06628v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.06628v1-abstract-full" style="display: none;"> Like most spiral galaxies, the Milky Way contains a population of blue, metal-poor globular clusters and another of red, metal-rich ones. Most of the latter belong to the bulge, and therefore they are poorly studied compared to the blue (halo) ones because they suffer higher extinction and larger contamination from field stars. These intrinsic difficulties, together with a lack of low-mass bulge globular clusters, are reasons to believe that their census is not complete yet. Indeed, a few new clusters have been confirmed in the last few years. One of them is VVV CL001, the subject of the present study. We present a new spectroscopic analysis of the recently confirmed globular cluster VVV CL001, made by means of MUSE@VLT integral field data. Individual spectra were extracted for stars in the VVV CL001 field. Radial velocities were derived by cross-correlation with synthetic templates. Coupled with PMs from the VVV survey, these data allow us to select 55 potential cluster members, for which we derive metallicities using the public code The Cannon. The mean radial velocity of the cluster is Vhelio = -324.9 +- 0.8 km/s,as estimated from 55 cluster members. This high velocity, together with a low metallicity [Fe/H] = -2.04 +- 0.02 dex suggests that VVV CL001 could be a very old cluster. The estimated distance is d = 8.23 +- 0.46 kpc, placing the cluster in the Galactic bulge. Furthermore, both its current position and the orbital parameters suggest that VVV CL001 is most probably a bulge globular cluster. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.06628v1-abstract-full').style.display = 'none'; document.getElementById('2204.06628v1-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 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">10 pages, 9 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/2108.11922">arXiv:2108.11922</a> <span> [<a href="https://arxiv.org/pdf/2108.11922">pdf</a>, <a href="https://arxiv.org/format/2108.11922">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stab2463">10.1093/mnras/stab2463 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Hidden in the Haystack: Low-luminosity globular clusters towards the Milky Way bulge </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=Zoccali%2C+M">M. Zoccali</a>, <a href="/search/astro-ph?searchtype=author&query=Saviane%2C+I">I. Saviane</a>, <a href="/search/astro-ph?searchtype=author&query=Valenti%2C+E">E. Valenti</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas-Arriagada%2C+A">A. Rojas-Arriagada</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=Hartke%2C+J">J. Hartke</a>, <a href="/search/astro-ph?searchtype=author&query=Carballo-Bello%2C+J+A">J. A. Carballo-Bello</a>, <a href="/search/astro-ph?searchtype=author&query=Navarrete%2C+C">C. Navarrete</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">M. Rejkuba</a>, <a href="/search/astro-ph?searchtype=author&query=Carvajal%2C+J+O">J. Olivares Carvajal</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="2108.11922v2-abstract-short" style="display: inline;"> Recent wide-area surveys have enabled us to study the Milky Way with unprecedented detail. Its inner regions, hidden behind dust and gas, have been partially unveiled with the arrival of near-IR photometric and spectroscopic datasets. Among recent discoveries, there is a population of low-mass globular clusters, known to be missing, especially towards the Galactic bulge. In this work, five new low… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.11922v2-abstract-full').style.display = 'inline'; document.getElementById('2108.11922v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.11922v2-abstract-full" style="display: none;"> Recent wide-area surveys have enabled us to study the Milky Way with unprecedented detail. Its inner regions, hidden behind dust and gas, have been partially unveiled with the arrival of near-IR photometric and spectroscopic datasets. Among recent discoveries, there is a population of low-mass globular clusters, known to be missing, especially towards the Galactic bulge. In this work, five new low-luminosity globular clusters located towards the bulge area are presented. They were discovered by searching for groups in the multi-dimensional space of coordinates, colours, and proper motions from the Gaia EDR3 catalogue and later confirmed with deeper VVV survey near-IR photometry. The clusters show well-defined red-giant branches and, in some cases, horizontal branches with their members forming a dynamically coherent structure in proper motion space. Four of them were confirmed by spectroscopic follow-up with the MUSE instrument on the ESO VLT. Photometric parameters were derived, and when available, metallicities, radial velocities and orbits were determined. The new clusters Gran 1 and 5 are bulge globular clusters, while Gran 2, 3, and 4 present halo-like properties. Preliminary orbits indicate that Gran 1 might be related to the Main Progenitor, or the so-called ''low-energy'' group, while Gran 2, 3 and 5 appear to follow the Gaia-Enceladus-Sausage. This study demonstrates that the Gaia proper motions, combined with the spectroscopic follow-up and colour-magnitude diagrams, are required to confirm the nature of cluster candidates towards the inner Galaxy. High stellar crowding and differential extinction may hide other low-luminosity clusters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.11922v2-abstract-full').style.display = 'none'; document.getElementById('2108.11922v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 11 figures, appendix: 7 figures, accepted for publication in MNRAS. Updated version with the correct orbit transformation applied. Fig. 11 and one sentence in Abstract, one in Sec. 4 and one in Summary were changed</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.00024">arXiv:2106.00024</a> <span> [<a href="https://arxiv.org/pdf/2106.00024">pdf</a>, <a href="https://arxiv.org/format/2106.00024">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/10.1051/0004-6361/202140436">10.1051/0004-6361/202140436 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CAPOS: The bulge Cluster APOgee Survey I. Overview and initial ASPCAP results </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Geisler%2C+D">Doug Geisler</a>, <a href="/search/astro-ph?searchtype=author&query=Villanova%2C+S">Sandro Villanova</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Connell%2C+J+E">Julia E. O'Connell</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=Bidin%2C+C+M">Christian Moni Bidin</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez-Trincado%2C+J+G">Jos茅 G. Fern谩ndez-Trincado</a>, <a href="/search/astro-ph?searchtype=author&query=Mu%C3%B1oz%2C+C">Cesar Mu帽oz</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">Dante Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Zoccali%2C+M">Manuela Zoccali</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas-Arriagada%2C+A">Alvaro Rojas-Arriagada</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=Catelan%2C+M">M谩rcio Catelan</a>, <a href="/search/astro-ph?searchtype=author&query=Mauro%2C+F">Francesco Mauro</a>, <a href="/search/astro-ph?searchtype=author&query=Cort%C3%A9s%2C+C">Crist铆an Cort茅s</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=Arentsen%2C+A">Anke Arentsen</a>, <a href="/search/astro-ph?searchtype=author&query=Starkenburg%2C+E">Else Starkenburg</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+N+F">Nicolas F. Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Tang%2C+B">Baitian Tang</a>, <a href="/search/astro-ph?searchtype=author&query=Parisi%2C+C">Celeste Parisi</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=Cunha%2C+K">Katia Cunha</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+V">Verne Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Majewski%2C+S+R">Steven R. Majewski</a> , et al. (17 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2106.00024v1-abstract-short" style="display: inline;"> Context. Bulge globular clusters (BGCs) are exceptional tracers of the formation and chemodynamical evolution of this oldest Galactic component. However, until now, observational difficulties have prevented us from taking full advantage of these powerful Galactic archeological tools. Aims. CAPOS, the bulge Cluster APOgee Survey, addresses this key topic by observing a large number of BGCs, most of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.00024v1-abstract-full').style.display = 'inline'; document.getElementById('2106.00024v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.00024v1-abstract-full" style="display: none;"> Context. Bulge globular clusters (BGCs) are exceptional tracers of the formation and chemodynamical evolution of this oldest Galactic component. However, until now, observational difficulties have prevented us from taking full advantage of these powerful Galactic archeological tools. Aims. CAPOS, the bulge Cluster APOgee Survey, addresses this key topic by observing a large number of BGCs, most of which have only been poorly studied previously. Even their most basic parameters, such as metallicity, [伪/Fe], and radial velocity, are generally very uncertain. We aim to obtain accurate mean values for these parameters, as well as abundances for a number of other elements, and explore multiple populations. In this first paper, we describe the CAPOS project and present initial results for seven BGCs. Methods. CAPOS uses the APOGEE-2S spectrograph observing in the H band to penetrate obscuring dust toward the bulge. For this initial paper, we use abundances derived from ASPCAP, the APOGEE pipeline. Results. We derive mean [Fe/H] values of $-$0.85$\pm$0.04 (Terzan 2), $-$1.40$\pm$0.05 (Terzan 4), $-$1.20$\pm$0.10 (HP 1), $-$1.40$\pm$0.07 (Terzan 9), $-$1.07$\pm$0.09 (Djorg 2), $-$1.06$\pm$0.06 (NGC 6540), and $-$1.11$\pm$0.04 (NGC 6642) from three to ten stars per cluster. We determine mean abundances for eleven other elements plus the mean [$伪$/Fe] and radial velocity. CAPOS clusters significantly increase the sample of well-studied Main Bulge globular clusters (GCs) and also extend them to lower metallicity. We reinforce the finding that Main Bulge and Main Disk GCs, formed in situ, have [Si/Fe] abundances slightly higher than their accreted counterparts at the same metallicity. We investigate multiple populations and find our clusters generally follow the light-element (anti)correlation trends of previous studies of GCs of similar metallicity. We finally explore the abundances ... <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.00024v1-abstract-full').style.display = 'none'; document.getElementById('2106.00024v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">27 pages, 10 figures, 5 tables. Abridged abstract. Accepted for publication in Astronomy & Astrophysics (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/2105.05825">arXiv:2105.05825</a> <span> [<a href="https://arxiv.org/pdf/2105.05825">pdf</a>, <a href="https://arxiv.org/format/2105.05825">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/10.1051/0004-6361/202140546">10.1051/0004-6361/202140546 <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. II. NGC6441, NGC6569, NGC6626 (M28), NGC6656 (M22), 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=Smith%2C+L+C">Leigh C. Smith</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=Minniti%2C+D">Dante Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Navarrete%2C+C">Camila Navarrete</a>, <a href="/search/astro-ph?searchtype=author&query=Borissova%2C+J">Jura Borissova</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=Ramos%2C+R+C">Rodrigo Contreras Ramos</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez-Trincado%2C+J+G">Jos茅 G. Fern谩ndez-Trincado</a>, <a href="/search/astro-ph?searchtype=author&query=Lopes%2C+C+E+F">Carlos E. Ferreira Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Gran%2C+F">Felipe Gran</a>, <a href="/search/astro-ph?searchtype=author&query=Garro%2C+E+R">Elisa R. Garro</a>, <a href="/search/astro-ph?searchtype=author&query=Geisler%2C+D">Doug Geisler</a>, <a href="/search/astro-ph?searchtype=author&query=Guo%2C+Z">Zhen Guo</a>, <a href="/search/astro-ph?searchtype=author&query=Hempel%2C+M">Maren Hempel</a>, <a href="/search/astro-ph?searchtype=author&query=Kerins%2C+E">Eamonn Kerins</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=Palma%2C+T">Tali Palma</a>, <a href="/search/astro-ph?searchtype=author&query=Ram%C3%ADrez%2C+K+P">Karla Pe帽a Ram铆rez</a>, <a href="/search/astro-ph?searchtype=author&query=Alegr%C3%ADa%2C+S+R">Sebasti谩n Ram铆rez Alegr铆a</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="2105.05825v1-abstract-short" style="display: inline;"> The Galactic globular clusters (GGCs) located in the inner regions of the Milky Way suffer from high extinction that makes their observation challenging. The VVV survey provides a way to explore these GGCs in the near-infrared where extinction effects are highly diminished. We conduct a search for variable stars in several inner GGCs, taking advantage of the unique multi-epoch, wide-field, near-in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.05825v1-abstract-full').style.display = 'inline'; document.getElementById('2105.05825v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.05825v1-abstract-full" style="display: none;"> The Galactic globular clusters (GGCs) located in the inner regions of the Milky Way suffer from high extinction that makes their observation challenging. The VVV survey provides a way to explore these GGCs in the near-infrared where extinction effects are highly diminished. We conduct a search for variable stars in several inner GGCs, taking advantage of the unique multi-epoch, wide-field, near-infrared photometry provided by the VVV survey. We are especially interested in detecting classical pulsators that will help us constrain the physical parameters of these GGCs. In this paper, the second of a series, we focus on NGC6656 (M22), NGC6626 (M28), NGC6569, and NGC6441; these four massive GGCs have known variable sources, but quite different metallicities. We also revisit 2MASS-GC02 and Terzan10, the two GGCs studied in the first paper of this series. We present an improved method and a new parameter that efficiently identify variable candidates in the GGCs. We also use the proper motions of those detected variable candidates and their positions in the sky and in the color-magnitude diagrams to assign membership to the GGCs. We identify and parametrize in the near-infrared numerous variable sources in the studied GGCs, cataloging tens of previously undetected variable stars. We recover many known classical pulsators in these clusters, including the vast majority of their fundamental mode RR Lyrae. We use these pulsators to obtain distances and extinctions toward these objects. Recalibrated period-luminosity-metallicity relations for the RR Lyrae bring the distances to these GGCs to a closer agreement with those reported by Gaia, except for NGC6441. Recovered proper motions for these GGCs also agree with those reported by Gaia, except for 2MASS-GC02, the most reddened GGC in our sample, where the VVV near-infrared measurements provide a more accurate determination of its proper motions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.05825v1-abstract-full').style.display = 'none'; document.getElementById('2105.05825v1-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 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A, 18 pages, 14 Figures, 9 Tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 651, A47 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2104.05865">arXiv:2104.05865</a> <span> [<a href="https://arxiv.org/pdf/2104.05865">pdf</a>, <a href="https://arxiv.org/format/2104.05865">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/stab1051">10.1093/mnras/stab1051 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> APOGEE view of the globular cluster NGC 6544 </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=Zoccali%2C+M">M. Zoccali</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas-Arriagada%2C+A">A. Rojas-Arriagada</a>, <a href="/search/astro-ph?searchtype=author&query=Saviane%2C+I">I. Saviane</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=Beaton%2C+R">R. Beaton</a>, <a href="/search/astro-ph?searchtype=author&query=Bizyaev%2C+D">D. Bizyaev</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R+E">R. E. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez-Trincado%2C+J+G">J. G. Fern谩ndez-Trincado</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Hern%C3%A1ndez%2C+D+A">D. A. Garc铆a-Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Geisler%2C+D">D. Geisler</a>, <a href="/search/astro-ph?searchtype=author&query=Lane%2C+R+R">R. R. Lane</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Bidin%2C+C+M">C. Moni Bidin</a>, <a href="/search/astro-ph?searchtype=author&query=Nitschelm%2C+C">C. Nitschelm</a>, <a href="/search/astro-ph?searchtype=author&query=Carvajal%2C+J+O">J. Olivares Carvajal</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+K">K. Pan</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas%2C+F+I">F. I. Rojas</a>, <a href="/search/astro-ph?searchtype=author&query=Villanova%2C+S">S. Villanova</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="2104.05865v1-abstract-short" style="display: inline;"> The second phase of the APOGEE survey is providing near-infrared, high-resolution, high signal-to-noise spectra of stars in the halo, disk, bar and bulge of the Milky Way. The near-infrared spectral window is especially important in the study of the Galactic bulge, where stars are obscured by the dust and gas of the disk in its line-of-sight. We present a chemical characterisation of the globular… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.05865v1-abstract-full').style.display = 'inline'; document.getElementById('2104.05865v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2104.05865v1-abstract-full" style="display: none;"> The second phase of the APOGEE survey is providing near-infrared, high-resolution, high signal-to-noise spectra of stars in the halo, disk, bar and bulge of the Milky Way. The near-infrared spectral window is especially important in the study of the Galactic bulge, where stars are obscured by the dust and gas of the disk in its line-of-sight. We present a chemical characterisation of the globular cluster NGC 6544 with high-resolution spectroscopy. The characterisation of the cluster chemical fingerprint, given its status of "interloper" towards the Galactic bulge and clear signatures of tidal disruption in its core is crucial for future chemical tagging efforts. Cluster members were selected from the DR16 of the APOGEE survey, using chemo-dynamical criteria of individual stars. A sample of 23 members of the cluster was selected. An analysis considering the intra-cluster abundance variations, known anticorrelations is given. According to the RGB content of the cluster, the iron content and $伪$-enhancement are [Fe/H] $= -1.44 \pm 0.04$ dex and [$伪$/Fe] $= 0.20 \pm 0.04$ dex, respectively. Cluster members show a significant spread in [Fe/H] and [Al/Fe] that is larger than expected based on measurement errors. An [Al/Fe] spread, signal of an Mg-Al anticorrelation is observed and used to constraint the cluster mass budget, along with C, N, Mg, Si, K, Ca, and Ce element variations are discussed. Across all the analysed evolutionary stages (RGB and AGB), about $\sim2/3$ (14 out of 23) show distinct chemical patterns, possibly associated with second-generation stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.05865v1-abstract-full').style.display = 'none'; document.getElementById('2104.05865v1-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 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 9 figures, MNRAS accepted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1904.10872">arXiv:1904.10872</a> <span> [<a href="https://arxiv.org/pdf/1904.10872">pdf</a>, <a href="https://arxiv.org/format/1904.10872">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201834986">10.1051/0004-6361/201834986 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Globular cluster candidates in the Galactic bulge: Gaia and VVV view of the latest discoveries </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=Zoccali%2C+M">M. Zoccali</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=Valenti%2C+E">E. Valenti</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas-Arriagada%2C+A">A. Rojas-Arriagada</a>, <a href="/search/astro-ph?searchtype=author&query=Carballo-Bello%2C+J+A">J. A. Carballo-Bello</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=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">M. Rejkuba</a>, <a href="/search/astro-ph?searchtype=author&query=Surot%2C+F">F. Surot</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1904.10872v1-abstract-short" style="display: inline;"> Thanks to the recent wide-area photometric surveys, the number of star cluster candidates have risen exponentially in the last few years. Most detections, however, are based only on the presence of an overdensity of stars in a given region, or an overdensity of variable stars, regardless of their distance. As candidates, their detection has not been dynamically confirmed. Therefore, it is currentl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.10872v1-abstract-full').style.display = 'inline'; document.getElementById('1904.10872v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1904.10872v1-abstract-full" style="display: none;"> Thanks to the recent wide-area photometric surveys, the number of star cluster candidates have risen exponentially in the last few years. Most detections, however, are based only on the presence of an overdensity of stars in a given region, or an overdensity of variable stars, regardless of their distance. As candidates, their detection has not been dynamically confirmed. Therefore, it is currently unknown how many, and which ones, of the published candidates, are true clusters, and which ones are chance alignments. We present a method to detect and confirm star clusters based on the spatial distribution, coherence in motion and appearance on the color-magnitude diagram. We explain and apply it to one new star cluster, and several candidate star clusters published in the literature. The presented method is based on data from the Second Data Release of Gaia complemented with data from the VISTA Variables in the V铆a L谩ctea survey for the innermost bulge regions. It consists of a nearest neighbors algorithm applied simultaneously over spatial coordinates, star color, and proper motions, in order to detect groups of stars that are close in the sky, move coherently and define narrow sequences in the color-magnitude diagram, such as a young main sequence or a red giant branch. When tested in the bulge area ($-10<\ell\ {\rm (deg)}<+10$; $-10<b\ {\rm (deg)}<+10$) the method successfully recovered several known young and old star clusters. We report here the detection of one new, likely old star cluster, while deferring the others to a forthcoming paper. Additionally, the code has been applied to the position of 93 candidate star clusters published in the literature. As a result, only two of them are confirmed as coherently moving groups of stars at their nominal positions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.10872v1-abstract-full').style.display = 'none'; document.getElementById('1904.10872v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">6 pages, 6 figures, A&A accepted. Appendix: 32 pages</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 628, A45 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1811.02265">arXiv:1811.02265</a> <span> [<a href="https://arxiv.org/pdf/1811.02265">pdf</a>, <a href="https://arxiv.org/format/1811.02265">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/sty3004">10.1093/mnras/sty3004 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> VVV-WIT-07: another Boyajian's star or a Mamajek's object? </p> <p class="authors"> <span class="search-hit">Authors:</span> <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>, <a href="/search/astro-ph?searchtype=author&query=Ivanov%2C+V+D">Valentin D. Ivanov</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=Gran%2C+F">Felipe Gran</a>, <a href="/search/astro-ph?searchtype=author&query=Baptista%2C+R">Raymundo Baptista</a>, <a href="/search/astro-ph?searchtype=author&query=Angeloni%2C+R">Rodolfo Angeloni</a>, <a href="/search/astro-ph?searchtype=author&query=Caceres%2C+C">Claudio Caceres</a>, <a href="/search/astro-ph?searchtype=author&query=Beamin%2C+J+C">Juan Carlos Beamin</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="1811.02265v1-abstract-short" style="display: inline;"> We report the discovery of VVV-WIT-07, an unique and intriguing variable source presenting a sequence of recurrent dips with a likely deep eclipse in July 2012. The object was found serendipitously in the near-IR data obtained by the VISTA Variables in the V铆a L谩ctea (VVV) ESO Public Survey. Our analysis is based on VVV variability, multicolor, and proper motion (PM) data. Complementary data from… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.02265v1-abstract-full').style.display = 'inline'; document.getElementById('1811.02265v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1811.02265v1-abstract-full" style="display: none;"> We report the discovery of VVV-WIT-07, an unique and intriguing variable source presenting a sequence of recurrent dips with a likely deep eclipse in July 2012. The object was found serendipitously in the near-IR data obtained by the VISTA Variables in the V铆a L谩ctea (VVV) ESO Public Survey. Our analysis is based on VVV variability, multicolor, and proper motion (PM) data. Complementary data from the VVV eXtended survey (VVVX) as well as archive data and spectroscopic follow-up observations aided in the analysis and interpretation of VVV-WIT-07. A search for periodicity in the VVV Ks-band light curve of VVV-WIT-07 results in two tentative periods at P~322 days and P~170 days. Colors and PM are consistent either with a reddened MS star or a pre-MS star in the foreground disk. The near-IR spectra of VVV-WIT-07 appear featureless, having no prominent lines in emission or absorption. Features found in the light curve of VVV-WIT-07 are similar to those seen in J1407 (Mamajek's object), a pre-MS K5 dwarf with a ring system eclipsing the star or, alternatively, to KIC 8462852 (Boyajian's star), an F3 IV/V star showing irregular and aperiodic dips in its light curve. Alternative scenarios, none of which is fully consistent with the available data, are also briefly discussed, including a young stellar object, a T Tauri star surrounded by clumpy dust structure, a main sequence star eclipsed by a nearby extended object, a self-eclipsing R CrB variable star, and even a long-period, high-inclination X-ray binary. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.02265v1-abstract-full').style.display = 'none'; document.getElementById('1811.02265v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 November, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">7 pages, 5 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/1807.04303">arXiv:1807.04303</a> <span> [<a href="https://arxiv.org/pdf/1807.04303">pdf</a>, <a href="https://arxiv.org/format/1807.04303">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/aacf90">10.3847/1538-4357/aacf90 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The VVV Survey RR Lyrae Population in the Galactic Centre Region </p> <p class="authors"> <span class="search-hit">Authors:</span> <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>, <a href="/search/astro-ph?searchtype=author&query=Gran%2C+F">Felipe Gran</a>, <a href="/search/astro-ph?searchtype=author&query=Zoccali%2C+M">Manuela Zoccali</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=Huijse%2C+P">Pablo Huijse</a>, <a href="/search/astro-ph?searchtype=author&query=Navarro%2C+M+G">Mar铆a Gabriela Navarro</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas-Arriagada%2C+%C3%81">脕lvaro Rojas-Arriagada</a>, <a href="/search/astro-ph?searchtype=author&query=Valenti%2C+E">Elena Valenti</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="1807.04303v1-abstract-short" style="display: inline;"> Deep near-IR images from the VVV Survey were used to search for RR Lyrae type ab (RRab) stars within 100' from the Galactic Centre (GC). A sample of 960 RRab stars were discovered. We use the reddening-corrected magnitudes in order to isolate RRab belonging to the GC. The mean period for our RRab sample is $P=0.5446$ days, yielding a mean metallicity of $[Fe/H] = -1.30$ dex and a median distance f… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.04303v1-abstract-full').style.display = 'inline'; document.getElementById('1807.04303v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1807.04303v1-abstract-full" style="display: none;"> Deep near-IR images from the VVV Survey were used to search for RR Lyrae type ab (RRab) stars within 100' from the Galactic Centre (GC). A sample of 960 RRab stars were discovered. We use the reddening-corrected magnitudes in order to isolate RRab belonging to the GC. The mean period for our RRab sample is $P=0.5446$ days, yielding a mean metallicity of $[Fe/H] = -1.30$ dex and a median distance from the Sun of $D=8.05$. We measure the RRab surface density using the less reddened region sampled here, finding $1000$ RRab/sq deg at a projected Galactocentric distance $R_G=1.6$ deg. This implies a large total mass ($M>10^9 M_\odot$) for the old and metal-poor population contained inside $R_G$. We measure accurate relative proper motions, from which we derive tangential velocity dispersions of $蟽V_l = 125.0$ and $蟽V_b = 124.1$ km/s along the Galactic longitude and latitude coordinates, respectively. The fact that these quantities are similar indicate that the bulk rotation of the RRab population is negligible, and implies that this population is supported by velocity dispersion. There are two main conclusions of this study. First, the population as a whole is no different from the outer bulge RRab, predominantly a metal-poor component that is shifted respect the Oosterhoff type I population defined by the globular clusters in the halo. Second, the RRab sample, as representative of the old and metal-poor stellar population in the region, have high velocity dispersions and zero rotation, suggesting a formation via dissipational collapse. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.04303v1-abstract-full').style.display = 'none'; document.getElementById('1807.04303v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 July, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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 figures, 2 tables, accepted in APJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1807.02065">arXiv:1807.02065</a> <span> [<a href="https://arxiv.org/pdf/1807.02065">pdf</a>, <a href="https://arxiv.org/format/1807.02065">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/aacd09">10.3847/1538-4357/aacd09 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Orbit of the new Milky Way Globular Cluster FSR1716 = VVV-GC05 </p> <p class="authors"> <span class="search-hit">Authors:</span> <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>, <a href="/search/astro-ph?searchtype=author&query=Fernandez-Trincado%2C+J+G">Jose G. Fernandez-Trincado</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso-Garcia%2C+J">Javier Alonso-Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Catelan%2C+M">Marcio Catelan</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=Hanke%2C+M">Michael Hanke</a>, <a href="/search/astro-ph?searchtype=author&query=Hempel%2C+M">Maren Hempel</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%ADaz%2C+E+M">Edmundo Moreno D铆az</a>, <a href="/search/astro-ph?searchtype=author&query=Perez-Villegas%2C+A">Angeles Perez-Villegas</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas-Arriagada%2C+A">Alvaro Rojas-Arriagada</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="1807.02065v1-abstract-short" style="display: inline;"> We use deep multi-epoch near-IR images of the VISTA Variables in the Via Lactea (VVV) Survey to measure proper motions (PMs) of stars in the Milky Way globular cluster FSR1716 = VVV-GC05. The color-magnitude diagram of this object, made using PM selected members, shows an extended horizontal branch, nine confirmed RR Lyrae members in the instability strip, and possibly several hotter stars extendi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.02065v1-abstract-full').style.display = 'inline'; document.getElementById('1807.02065v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1807.02065v1-abstract-full" style="display: none;"> We use deep multi-epoch near-IR images of the VISTA Variables in the Via Lactea (VVV) Survey to measure proper motions (PMs) of stars in the Milky Way globular cluster FSR1716 = VVV-GC05. The color-magnitude diagram of this object, made using PM selected members, shows an extended horizontal branch, nine confirmed RR Lyrae members in the instability strip, and possibly several hotter stars extending to the blue. Based on the fundamental-mode (ab-type) RR Lyrae stars that move coherently with the cluster, we confirmed that FSR1716 is an Oosterhoff I globular cluster with a mean period Pab = 0.574 days. Intriguingly, we detect tidal extensions to both sides of this cluster in the spatial distribution of PM selected member stars. Also, one of the confirmed RRabs is located 11 arcmin in projection from the cluster center, suggesting that FSR1716 may be losing stars due to the gravitational interaction with the Galaxy. We also measure radial velocities (RVs) for five cluster red giants selected using the PMs. The combination of RVs and PMs allow us to compute for the first time the orbit of this globular cluster, using an updated Galactic potential. The orbit results to be confined within |Zmax | < 2.0 kpc, and has eccentricity 0.4 < e < 0.6, with perigalactic distance 1.5 < Rperi (kpc) < 2.3, and apogalactic distance 5.3 < Rapo (kpc) < 6.4. We conclude that, in agreement with its relatively low metallicity ([Fe/H]= -1.4 dex), this is an inner halo globular cluster plunging into the disk of the Galaxy. As such, this is a unique object to test the dynamical processes that contribute to the disruption of Galactic globular clusters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.02065v1-abstract-full').style.display = 'none'; document.getElementById('1807.02065v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 July, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">6 figures, 4 tables, accepted in APJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1709.07919">arXiv:1709.07919</a> <span> [<a href="https://arxiv.org/pdf/1709.07919">pdf</a>, <a href="https://arxiv.org/format/1709.07919">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/10.1051/0004-6361/201731462">10.1051/0004-6361/201731462 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Proper motions in the VVV Survey: Results for more than 15 million stars across NGC 6544 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ramos%2C+R+C">R. Contreras Ramos</a>, <a href="/search/astro-ph?searchtype=author&query=Zoccali%2C+M">M. Zoccali</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas%2C+F">F. Rojas</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas-Arriagada%2C+A">A. Rojas-Arriagada</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%A1rate%2C+M">M. G谩rate</a>, <a href="/search/astro-ph?searchtype=author&query=Huijse%2C+P">P. Huijse</a>, <a href="/search/astro-ph?searchtype=author&query=Gran%2C+F">F. Gran</a>, <a href="/search/astro-ph?searchtype=author&query=Soto%2C+M">M. Soto</a>, <a href="/search/astro-ph?searchtype=author&query=Valcarce%2C+A+A+R">A. A. R. Valcarce</a>, <a href="/search/astro-ph?searchtype=author&query=Est%C3%A9vez%2C+P+A">P. A. Est茅vez</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="1709.07919v1-abstract-short" style="display: inline;"> Context: In the last six years, the VVV survey mapped 562 sq. deg. across the bulge and southern disk of the Galaxy. However, a detailed study of these regions, which includes $\sim 36$ globular clusters (GCs) and thousands of open clusters is by no means an easy challenge. High differential reddening and severe crowding along the line of sight makes highly hamper to reliably distinguish stars bel… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1709.07919v1-abstract-full').style.display = 'inline'; document.getElementById('1709.07919v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1709.07919v1-abstract-full" style="display: none;"> Context: In the last six years, the VVV survey mapped 562 sq. deg. across the bulge and southern disk of the Galaxy. However, a detailed study of these regions, which includes $\sim 36$ globular clusters (GCs) and thousands of open clusters is by no means an easy challenge. High differential reddening and severe crowding along the line of sight makes highly hamper to reliably distinguish stars belonging to different populations and/or systems. Aims: The aim of this study is to separate stars that likely belong to the Galactic GC NGC 6544 from its surrounding field by means of proper motion (PM) techniques. Methods: This work was based upon a new astrometric reduction method optimized for images of the VVV survey. Results: Photometry over the six years baseline of the survey allowed us to obtain a mean precision of $\sim0.51$ mas/yr, in each PM coordinate, for stars with Ks < 15 mag. In the area studied here, cluster stars separate very well from field stars, down to the main sequence turnoff and below, allowing us to derive for the first time the absolute PM of NGC 6544. Isochrone fitting on the clean and differential reddening corrected cluster color magnitude diagram yields an age of $\sim$ 11-13 Gyr, and metallicity [Fe/H] = -1.5 dex, in agreement with previous studies restricted to the cluster core. We were able to derive the cluster orbit assuming an axisymmetric model of the Galaxy and conclude that NGC 6544 is likely a halo GC. We have not detected tidal tail signatures associated to the cluster, but a remarkable elongation in the galactic center direction has been found. The precision achieved in the PM determination also allows us to separate bulge stars from foreground disk stars, enabling the kinematical selection of bona fide bulge stars across the whole survey area. Our results show that VVV data is perfectly suitable for this kind of analysis. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1709.07919v1-abstract-full').style.display = 'none'; document.getElementById('1709.07919v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 September, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 12 figures, accepted in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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/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/1610.04689">arXiv:1610.04689</a> <span> [<a href="https://arxiv.org/pdf/1610.04689">pdf</a>, <a href="https://arxiv.org/format/1610.04689">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8205/830/1/L14">10.3847/2041-8205/830/1/L14 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery of RR Lyrae Stars in the Nuclear Bulge of the Milky Way </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Ramos%2C+R+C">R. Contreras Ramos</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=Gonzalez%2C+O+A">O. A. Gonzalez</a>, <a href="/search/astro-ph?searchtype=author&query=Valenti%2C+E">E. Valenti</a>, <a href="/search/astro-ph?searchtype=author&query=Gran%2C+F">F. Gran</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="1610.04689v1-abstract-short" style="display: inline;"> Galactic nuclei, like the one of the Milky Way, are extreme places with high stellar densities and, in most cases, hosting a supermassive black hole. One of the scenarios proposed for the formation of the Galactic nucleus is by merging of primordial globular clusters (Capuzzo-Dolcetta 1993). An implication of this model is that this region should host stars characteristically found in old Milky Wa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1610.04689v1-abstract-full').style.display = 'inline'; document.getElementById('1610.04689v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1610.04689v1-abstract-full" style="display: none;"> Galactic nuclei, like the one of the Milky Way, are extreme places with high stellar densities and, in most cases, hosting a supermassive black hole. One of the scenarios proposed for the formation of the Galactic nucleus is by merging of primordial globular clusters (Capuzzo-Dolcetta 1993). An implication of this model is that this region should host stars characteristically found in old Milky Way globular clusters. RR Lyrae stars are primary distance indicators, well known representatives of old and metal-poor stellar populations, and therefore regularly found in globular clusters. Here we report the discovery of a dozen RR Lyrae ab-type stars in the vicinity of the Galactic center, i.e. in the so-called nuclear stellar bulge of the Milky Way. This discovery provides the first direct observational evidence that the Galactic nuclear stellar bulge contains ancient stars (>10 Gyr old). Based on this we conclude that merging globular clusters likely contributed to building-up the high stellar density in the nuclear stellar bulge of the Milky Way. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1610.04689v1-abstract-full').style.display = 'none'; document.getElementById('1610.04689v1-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 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">Accepted for publication on ApJL, 4 pages, 4 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/1604.01336">arXiv:1604.01336</a> <span> [<a href="https://arxiv.org/pdf/1604.01336">pdf</a>, <a href="https://arxiv.org/format/1604.01336">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/10.1051/0004-6361/201527511">10.1051/0004-6361/201527511 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Mapping the outer bulge with RRab stars from the VVV Survey </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=Zoccali%2C+M">M. Zoccali</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=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=Elorrieta%2C+F">F. Elorrieta</a>, <a href="/search/astro-ph?searchtype=author&query=Eyheramendy%2C+S">S. Eyheramendy</a>, <a href="/search/astro-ph?searchtype=author&query=Jord%C3%A1n%2C+A">A. 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="1604.01336v1-abstract-short" style="display: inline;"> The VISTA Variables in the V铆a L谩ctea (VVV) is a near-IR time-domain survey of the Galactic bulge and southern plane. One of the main goals of this survey is to reveal the 3D structure of the Milky Way through their variable stars. Particularly the RR Lyrae stars have been massively discovered in the inner regions of the bulge ($-8^\circ \lesssim b \lesssim -1^\circ$) by optical surveys such as OG… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.01336v1-abstract-full').style.display = 'inline'; document.getElementById('1604.01336v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1604.01336v1-abstract-full" style="display: none;"> The VISTA Variables in the V铆a L谩ctea (VVV) is a near-IR time-domain survey of the Galactic bulge and southern plane. One of the main goals of this survey is to reveal the 3D structure of the Milky Way through their variable stars. Particularly the RR Lyrae stars have been massively discovered in the inner regions of the bulge ($-8^\circ \lesssim b \lesssim -1^\circ$) by optical surveys such as OGLE and MACHO but leaving an unexplored window of more than $\sim 47$ sq deg ($-10.0^\circ \lesssim \ell \lesssim +10.7^\circ$ and $-10.3^\circ \lesssim b \lesssim -8.0^\circ$) observed by the VVV Survey. Our goal is to characterize the RR Lyrae stars in the outer bulge in terms of their periods, amplitudes, Fourier coefficients, and distances, in order to evaluate the 3D structure of the bulge in this area. The distance distribution of RR Lyrae stars will be compared to the one of red clump stars that is known to trace a X-shaped structure in order to determine if these two different stellar populations share the same Galactic distribution. We report the detection of more than 1000 RR Lyrae ab-type stars in the VVV Survey located in the outskirts of the Galactic bulge. Some of them are possibly associated with the Sagittarius Dwarf Spheroidal Galaxy. We calculated colors, reddening, extinction, and distances of the detected RR Lyrae stars in order to determine the outer bulge 3D structure. Our main result is that, at the low galactic latitudes mapped here, the RR Lyrae stars trace a centrally concentrated spheroidal distribution. This is a noticeably different spatial distribution to the one traced by red clump stars known to follow a bar and X-shape structure. We estimate the completeness of our RRab sample in $80\%$ for $K_{\rm s}\lesssim15$ mag. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.01336v1-abstract-full').style.display = 'none'; document.getElementById('1604.01336v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 April, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">26 pages, 8 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 591, A145 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1508.06957">arXiv:1508.06957</a> <span> [<a href="https://arxiv.org/pdf/1508.06957">pdf</a>, <a href="https://arxiv.org/ps/1508.06957">ps</a>, <a href="https://arxiv.org/format/1508.06957">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/10.1088/2041-8205/810/2/L20">10.1088/2041-8205/810/2/L20 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> VVV Survey Observations of a Microlensing Stellar Mass Black Hole Candidate in the Field of the Globular Cluster NGC 6553 </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=Ramos%2C+R+C">R. Contreras Ramos</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=Anguita%2C+T">T. Anguita</a>, <a href="/search/astro-ph?searchtype=author&query=Catelan%2C+M">M. Catelan</a>, <a href="/search/astro-ph?searchtype=author&query=Gran%2C+F">F. Gran</a>, <a href="/search/astro-ph?searchtype=author&query=Motta%2C+V">V. Motta</a>, <a href="/search/astro-ph?searchtype=author&query=Muro%2C+G">G. Muro</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas%2C+K">K. Rojas</a>, <a href="/search/astro-ph?searchtype=author&query=Saito%2C+R+K">R. 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="1508.06957v1-abstract-short" style="display: inline;"> We report the discovery of a large timescale candidate microlensing event of a bulge stellar source based on near-infrared observations with the VISTA Variables in the Via Lactea Survey (VVV). The new microlensing event is projected only 3.5 arcmin away from the center of the globular cluster NGC 6553. The source appears to be a bulge giant star with magnitude Ks = 13.52, based on the position in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1508.06957v1-abstract-full').style.display = 'inline'; document.getElementById('1508.06957v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1508.06957v1-abstract-full" style="display: none;"> We report the discovery of a large timescale candidate microlensing event of a bulge stellar source based on near-infrared observations with the VISTA Variables in the Via Lactea Survey (VVV). The new microlensing event is projected only 3.5 arcmin away from the center of the globular cluster NGC 6553. The source appears to be a bulge giant star with magnitude Ks = 13.52, based on the position in the color-magnitude diagram. The foreground lens may be located in the globular cluster, which has well-known parameters such as distance and proper motions. If the lens is a cluster member, we can directly estimate its mass simply following Paczynski et al. (1996) which is a modified version of the more general case due to Refsdal. In that case, the lens would be a massive stellar remnant, with M = 1.5-3.5 Msun. If the blending fraction of the microlensing event appears to be small, and this lens would represent a good isolated black hole (BH) candidate, that would be the oldest BH known. Alternative explanations (with a larger blending fraction) also point to a massive stellar remnant if the lens is located in the Galactic disk and does not belong to the globular cluster. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1508.06957v1-abstract-full').style.display = 'none'; document.getElementById('1508.06957v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 August, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">5 pages, 3 figures, 1 table, accepted for publication in ApJL</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1502.01358">arXiv:1502.01358</a> <span> [<a href="https://arxiv.org/pdf/1502.01358">pdf</a>, <a href="https://arxiv.org/format/1502.01358">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/10.1088/2041-8205/802/1/L4">10.1088/2041-8205/802/1/L4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Clustered Cepheid Variables 90 kiloparsec from the Galactic Center </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chakrabarti%2C+S">Sukanya Chakrabarti</a>, <a href="/search/astro-ph?searchtype=author&query=Saito%2C+R">Roberto Saito</a>, <a href="/search/astro-ph?searchtype=author&query=Quillen%2C+A">Alice Quillen</a>, <a href="/search/astro-ph?searchtype=author&query=Gran%2C+F">Felipe Gran</a>, <a href="/search/astro-ph?searchtype=author&query=Klein%2C+C">Christopher Klein</a>, <a href="/search/astro-ph?searchtype=author&query=Blitz%2C+L">Leo Blitz</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="1502.01358v1-abstract-short" style="display: inline;"> Distant regions close to the plane of our Galaxy are largely unexplored by optical surveys as they are hidden by dust. We have used near-infrared data (that minimizes dust obscuration) from the ESO Public survey VISTA Variables of the Via Lactea (VVV) (Minniti et al. 2011; Saito et al. 2012; henceforth S12) to search for distant stars at low latitudes. We have discovered four Cepheid variables wit… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1502.01358v1-abstract-full').style.display = 'inline'; document.getElementById('1502.01358v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1502.01358v1-abstract-full" style="display: none;"> Distant regions close to the plane of our Galaxy are largely unexplored by optical surveys as they are hidden by dust. We have used near-infrared data (that minimizes dust obscuration) from the ESO Public survey VISTA Variables of the Via Lactea (VVV) (Minniti et al. 2011; Saito et al. 2012; henceforth S12) to search for distant stars at low latitudes. We have discovered four Cepheid variables within an angular extent of one degree centered at Galactic longitude of $l = -27.4^\circ$ and Galactic latitude of $b = -1.08 ^\circ$. We use the tightly constrained period-luminosity relationship that these pulsating stars obey (Persson et al. 2004; Matsunaga et al. 2011) to derive distances. We infer an average distance to these Cepheid variables of 90 kpc. The Cepheid variables are highly clustered in angle (within one degree) and in distance (the standard deviation of the distances is 12 kpc). They are at an average distance of $\sim 2~\rm kpc$ from the plane and their maximum projected separation is $\sim 1~ \rm kpc$. These young ($\sim$ 100 Myr old), pulsating stars (Bono et al. 2005) are unexpected at such large distances from the Galactic disk, which terminates at $\sim$ 15 kpc (Minniti et al. 2011). The highly clustered nature in distance and angle of the Cepheid variables suggests that the stars may be associated with a dwarf galaxy, one that was earlier predicted by a dynamical analysis (Chakrabarti \& Blitz 2009). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1502.01358v1-abstract-full').style.display = 'none'; document.getElementById('1502.01358v1-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">accepted to ApJL</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/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/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/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> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 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