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</div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.06924">arXiv:2409.06924</a> <span> [<a href="https://arxiv.org/pdf/2409.06924">pdf</a>, <a href="https://arxiv.org/format/2409.06924">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> The young exoplanetary system TOI-4562: Confirming the presence of a third body in the system </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Fermiano%2C+V">V. Fermiano</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=Ivanov%2C+V+D">V. D. Ivanov</a>, <a href="/search/astro-ph?searchtype=author&query=Caceres%2C+C">C. Caceres</a>, <a href="/search/astro-ph?searchtype=author&query=Almeida%2C+L+A">L. A. Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Aires%2C+J">J. Aires</a>, <a href="/search/astro-ph?searchtype=author&query=Beamin%2C+J+C">J. C. Beamin</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+T">T. Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade%2C+L">L. Andrade</a>, <a href="/search/astro-ph?searchtype=author&query=Borges%2C+B+W">B. W. Borges</a>, <a href="/search/astro-ph?searchtype=author&query=de+Almeida%2C+L">L. de Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Jablonski%2C+F">F. Jablonski</a>, <a href="/search/astro-ph?searchtype=author&query=Schlindwein%2C+W">W. Schlindwein</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="2409.06924v1-abstract-short" style="display: inline;"> Young planetary systems represent an opportunity to investigate the early stages of (exo)planetary formation because the gravitational interactions have not yet significantly changed the initial configuration of the system. TOI-4562 b is a highly eccentric temperate Jupiter analogue orbiting a young F7V-type star of $<700$ Myr in age with an orbital period of $P_{orb} \sim 225$ days and an eccentr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.06924v1-abstract-full').style.display = 'inline'; document.getElementById('2409.06924v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.06924v1-abstract-full" style="display: none;"> Young planetary systems represent an opportunity to investigate the early stages of (exo)planetary formation because the gravitational interactions have not yet significantly changed the initial configuration of the system. TOI-4562 b is a highly eccentric temperate Jupiter analogue orbiting a young F7V-type star of $<700$ Myr in age with an orbital period of $P_{orb} \sim 225$ days and an eccentricity of $e=0.76$, and is one of the largest known exoplanets to have formed in situ. We observed a new transit of TOI-4562 b using the 0.6-m Zeiss telescope at the Pico dos Dias Observatory (OPD/LNA) in Minas Gerais, Brazil, and combine our data with Transiting Exoplanet Survey Satellite (TESS) and archive data, with the aim being to improve the ephemerides of this interesting system. The $O-C$ diagram for the new ephemeris is consistent with the presence of a giant planet in an outer orbit around TOI-4562. TOI-4562 c is a planet with a mass of $M=5.77 M_{Jup}$, an orbital period of $P_{orb}= 3990$ days, and a semi-major axis of $a = 5.219$ AU. We report the discovery of TOI-4562 c, the exoplanet with the longest orbital period discovered to date via the transit timing variation (TTV) method. The TOI-4562 system is in the process of violent evolution with intense dynamical changes - judging by its young age and high eccentricity - and is therefore a prime target for studies of formation and evolution of planetary systems. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.06924v1-abstract-full').style.display = 'none'; document.getElementById('2409.06924v1-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 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">5 pages and 3 figures (+ appendix). Accepted for publication in Astronomy & Astrophysics, Letters to the Editor</span> </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/2404.05420">arXiv:2404.05420</a> <span> [<a href="https://arxiv.org/pdf/2404.05420">pdf</a>, <a href="https://arxiv.org/format/2404.05420">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"> Accretion Funnel Reconfiguration during an Outburst in a Young Stellar Object: EX Lupi </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Singh%2C+K">Koshvendra Singh</a>, <a href="/search/astro-ph?searchtype=author&query=Ninan%2C+J+P">Joe P. Ninan</a>, <a href="/search/astro-ph?searchtype=author&query=Romanova%2C+M+M">Marina M. Romanova</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+D+A+H">David A. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Ojha%2C+D+K">Devendra K. Ojha</a>, <a href="/search/astro-ph?searchtype=author&query=Ghosh%2C+A">Arpan Ghosh</a>, <a href="/search/astro-ph?searchtype=author&query=Monson%2C+A">Andrew Monson</a>, <a href="/search/astro-ph?searchtype=author&query=Schramm%2C+M">Malte Schramm</a>, <a href="/search/astro-ph?searchtype=author&query=Sharma%2C+S">Saurabh Sharma</a>, <a href="/search/astro-ph?searchtype=author&query=Reichart%2C+D+E">Daniel E. Reichart</a>, <a href="/search/astro-ph?searchtype=author&query=Mikolajewska%2C+J">Joanna Mikolajewska</a>, <a href="/search/astro-ph?searchtype=author&query=Beamin%2C+J+C">Juan Carlos Beamin</a>, <a href="/search/astro-ph?searchtype=author&query=Borissova%2C+J">J. Borissova</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=Kouprianov%2C+V+V">Vladimir V. Kouprianov</a>, <a href="/search/astro-ph?searchtype=author&query=Hambsch%2C+F">Franz-Josef Hambsch</a>, <a href="/search/astro-ph?searchtype=author&query=Pearce%2C+A">Andrew Pearce</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="2404.05420v1-abstract-short" style="display: inline;"> EX Lupi, a low-mass young stellar object, went into an accretion-driven outburst in March of 2022. The outburst caused a sudden phase change of ~ 112$^{\circ}$ $\pm$ 5$^{\circ}$ in periodically oscillating multiband lightcurves. Our high resolution spectra obtained with HRS on SALT also revealed a consistent phase change in the periodically varying radial velocities, along with an increase in the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.05420v1-abstract-full').style.display = 'inline'; document.getElementById('2404.05420v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.05420v1-abstract-full" style="display: none;"> EX Lupi, a low-mass young stellar object, went into an accretion-driven outburst in March of 2022. The outburst caused a sudden phase change of ~ 112$^{\circ}$ $\pm$ 5$^{\circ}$ in periodically oscillating multiband lightcurves. Our high resolution spectra obtained with HRS on SALT also revealed a consistent phase change in the periodically varying radial velocities, along with an increase in the radial velocity amplitude of various emission lines. The phase change and increase of radial velocity amplitude morphologically translates to a change in the azimuthal and latitudinal location of the accretion hotspot over the stellar surface, which indicates a reconfiguration of the accretion funnel geometry. Our 3D MHD simulations reproduce the phase change for EX Lupi. To explain the observations we explored the possibility of forward shifting of the dipolar accretion funnel as well as the possibility of an emergence of a new accretion funnel. During the outburst, we also found evidence of the hotspot's morphology extending azimuthally, asymmetrically with a leading hot edge and cold tail along the stellar rotation. Our high cadence photometry showed that the accretion flow has clumps. We also detected possible clumpy accretion events in the HRS spectra, that showed episodically highly blue-shifted wings in the Ca II IRT and Balmer H lines. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.05420v1-abstract-full').style.display = 'none'; document.getElementById('2404.05420v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in The Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.10158">arXiv:2312.10158</a> <span> [<a href="https://arxiv.org/pdf/2312.10158">pdf</a>, <a href="https://arxiv.org/format/2312.10158">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"> A Benchmark White Dwarf-Ultracool Dwarf Wide Field Binary </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+T">Thiago Ferreira</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>, <a href="/search/astro-ph?searchtype=author&query=Mej%C3%ADas%2C+A">Andrea Mej铆as</a>, <a href="/search/astro-ph?searchtype=author&query=Caceres%2C+C">Claudio Caceres</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=Beam%C3%ADn%2C+J+C">Juan Carlos Beam铆n</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=Gomez%2C+M">Mat铆as Gomez</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=Ivanov%2C+V+D">Valentin D. Ivanov</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.10158v1-abstract-short" style="display: inline;"> We present the discovery and multi-wavelength characterisation of VVV J1438-6158 AB, a new field wide-binary system consisting of a 4.6(+5.5-2.4) Gyr and Teff = 9500+/-125 K DA white dwarf (WD) and a Teff = 2400+/-50 K M8 ultracool dwarf (UCD). The projected separation of the system is a = 1236.73 au (~13.8"), and although along the line-of-sight towards the Scorpius-Centaurus (Sco-Cen) stellar as… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.10158v1-abstract-full').style.display = 'inline'; document.getElementById('2312.10158v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.10158v1-abstract-full" style="display: none;"> We present the discovery and multi-wavelength characterisation of VVV J1438-6158 AB, a new field wide-binary system consisting of a 4.6(+5.5-2.4) Gyr and Teff = 9500+/-125 K DA white dwarf (WD) and a Teff = 2400+/-50 K M8 ultracool dwarf (UCD). The projected separation of the system is a = 1236.73 au (~13.8"), and although along the line-of-sight towards the Scorpius-Centaurus (Sco-Cen) stellar association, VVV J1438-6158 AB is likely to be a field star, from a kinematic 6D probabilistic analysis. We estimated the physical, and dynamical parameters of both components via interpolations with theoretical models and evolutionary tracks, which allowed us to retrieve a mass of 0.62+/-0.18 MSun for the WD, and a mass of 98.5+/-6.2 MJup (~0.094+/-0.006 MSun) for the UCD. The radii of the two components were also estimated at 0.01309+/-0.0003 RSun and 1.22+/-0.05 RJup, respectively. VVV J1438-6158 AB stands out as a benchmark system for comprehending the evolution of WDs and low-mass companions given its status as one of the most widely separated WD+UCD systems known to date, which likely indicates that both components may have evolved independently of each other, and also being characterised by a large mass-ratio (q = 0.15+/-0.04), which likely indicates a formation pathway similar to that of stellar binary systems. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.10158v1-abstract-full').style.display = 'none'; document.getElementById('2312.10158v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in MNRAS, 11 pages, 6 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.01593">arXiv:2311.01593</a> <span> [<a href="https://arxiv.org/pdf/2311.01593">pdf</a>, <a href="https://arxiv.org/format/2311.01593">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> VVV-WIT-12 and its fashionable nebula: a four year long period Young Stellar Object with a light echo? </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=Stecklum%2C+B">Bringfried Stecklum</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">Dante Minniti</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=Guo%2C+Z">Zhen Guo</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=Fraga%2C+L">Luciano Fraga</a>, <a href="/search/astro-ph?searchtype=author&query=Navarete%2C+F">Felipe Navarete</a>, <a href="/search/astro-ph?searchtype=author&query=Beam%C3%ADn%2C+J+C">Juan Carlos Beam铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Morris%2C+C">Calum Morris</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.01593v1-abstract-short" style="display: inline;"> We report the serendipitous discovery of VVV-WIT-12, an unusual variable source that seems to induce variability in its surrounding nebula. The source belongs to the rare objects that we call WITs (short for What Is This?) discovered within the VISTA Variables in the V铆a L谩ctea (VVV) survey. VVV-WIT-12 was discovered during a pilot search for light echoes from distant Supernovae (SNe) in the Milky… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.01593v1-abstract-full').style.display = 'inline'; document.getElementById('2311.01593v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.01593v1-abstract-full" style="display: none;"> We report the serendipitous discovery of VVV-WIT-12, an unusual variable source that seems to induce variability in its surrounding nebula. The source belongs to the rare objects that we call WITs (short for What Is This?) discovered within the VISTA Variables in the V铆a L谩ctea (VVV) survey. VVV-WIT-12 was discovered during a pilot search for light echoes from distant Supernovae (SNe) in the Milky Way using the near-IR images of the VVV survey. This source has an extremely red spectral energy distribution, consistent with a very reddened ($A_V \sim 100$ mag) long period variable star ($P\sim1525$ days). Furthermore, it is enshrouded in a nebula that changes brightness and color with time, apparently in synch with the central source variations. The near-IR light curve and complementary follow-up spectroscopy observations are consistent with a variable Young Stellar Object (YSO) illuminating its surrounding nebula. In this case the source periodic variation along the cycles produces an unprecedented light echo in the different regions of the nebula. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.01593v1-abstract-full').style.display = 'none'; document.getElementById('2311.01593v1-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 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in The Astrophysical Journal Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.00786">arXiv:2203.00786</a> <span> [<a href="https://arxiv.org/pdf/2203.00786">pdf</a>, <a href="https://arxiv.org/format/2203.00786">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/10.1051/0004-6361/202141759">10.1051/0004-6361/202141759 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> VVVX near-IR photometry for 99 low-mass stars in the Gaia EDR3 Catalog of Nearby Stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mej%C3%ADas%2C+A">Andrea Mej铆as</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">Dante Minniti</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=Beam%C3%ADn%2C+J+C">Juan Carlos Beam铆n</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=Solano%2C+E">Enrique Solano</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="2203.00786v1-abstract-short" style="display: inline;"> Red dwarf stars, which represent 75% of stars in the Milky Way, can be studied in great detail in the solar neighborhood where the sample is more complete. We intend to better characterize red dwarf candidates selected from the Gaia Catalog of Nearby Stars using optical and near-infrared photometry from the VVVX Survey, DECaPS, Pan-STARRS, and WISE. We performed a cross-matching procedure among th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.00786v1-abstract-full').style.display = 'inline'; document.getElementById('2203.00786v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.00786v1-abstract-full" style="display: none;"> Red dwarf stars, which represent 75% of stars in the Milky Way, can be studied in great detail in the solar neighborhood where the sample is more complete. We intend to better characterize red dwarf candidates selected from the Gaia Catalog of Nearby Stars using optical and near-infrared photometry from the VVVX Survey, DECaPS, Pan-STARRS, and WISE. We performed a cross-matching procedure among the positions of a color-selected sample of M dwarfs in the VVVX Survey and the Gaia EDR3 sub-catalog of nearby stars. We explored their stellar parameters and spectral types using VOSA. Radii were also obtained using the Stefan-Boltzmann equation. Masses and ages were computed for some of the objects using evolutionary tracks and isochrones. Additional mass estimations were obtained with the MKs - M* relation. We then validated our results for the stellar parameters of two of our objects with spectra obtained with the TripleSpec instrument at the SOAR telescope, as well as those of our total amount of stars through a direct comparison with an independent sample from the literature. We revised the objects in our sample and compared their proper motion vectors with other sources within 30" to identify possible companions and probed their RUWE values to identify unresolved companions. We present a catalog of physical parameters for 99 low-mass objects with distances from 43.2 to 111.3 pc. Teffs range from 2500 to 3400 K, with the majority of stars in the sample compatible with being M4 dwarfs. We obtained a good agreement between the stellar parameters computed with VOSA and the estimations from observed spectra, also when comparing with an independent sample from the literature. The distribution of masses obtained with VOSA is concentrated toward the very low-mass regime. Eight objects present values of RUWE >= 1.4 and seven are consistent with being part of a binary system. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.00786v1-abstract-full').style.display = 'none'; document.getElementById('2203.00786v1-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 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 9 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> 85-00 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 660, A131 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.05731">arXiv:2012.05731</a> <span> [<a href="https://arxiv.org/pdf/2012.05731">pdf</a>, <a href="https://arxiv.org/format/2012.05731">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="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/staa3836">10.1093/mnras/staa3836 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Serendipitous discovery of a dusty disc around WDJ181417.84-735459.83 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Egea%2C+E+G">E. Gonz谩lez Egea</a>, <a href="/search/astro-ph?searchtype=author&query=Raddi%2C+R">R. Raddi</a>, <a href="/search/astro-ph?searchtype=author&query=Koester%2C+D">D. Koester</a>, <a href="/search/astro-ph?searchtype=author&query=Rogers%2C+L+K">L. K. Rogers</a>, <a href="/search/astro-ph?searchtype=author&query=Marocco%2C+F">F. Marocco</a>, <a href="/search/astro-ph?searchtype=author&query=Cooper%2C+W+J">W. J. Cooper</a>, <a href="/search/astro-ph?searchtype=author&query=Beamin%2C+J+C">J. C. Beamin</a>, <a href="/search/astro-ph?searchtype=author&query=Burningham%2C+B">B. Burningham</a>, <a href="/search/astro-ph?searchtype=author&query=Day-Jones%2C+A">A. Day-Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Forbrich%2C+J">J. Forbrich</a>, <a href="/search/astro-ph?searchtype=author&query=Pinfield%2C+D+J">D. J. Pinfield</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="2012.05731v2-abstract-short" style="display: inline;"> Spectroscopic observations of white dwarfs reveal that many of them are polluted by exoplanetary material, whose bulk composition can be uniquely probed this way. We present a spectroscopic and photometric analysis of the DA white dwarf WDJ181417.84$-$735459.83, an object originally identified to have a strong infrared excess in the 2MASS and WISE catalogues that we confirmed to be intrinsic to th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.05731v2-abstract-full').style.display = 'inline'; document.getElementById('2012.05731v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.05731v2-abstract-full" style="display: none;"> Spectroscopic observations of white dwarfs reveal that many of them are polluted by exoplanetary material, whose bulk composition can be uniquely probed this way. We present a spectroscopic and photometric analysis of the DA white dwarf WDJ181417.84$-$735459.83, an object originally identified to have a strong infrared excess in the 2MASS and WISE catalogues that we confirmed to be intrinsic to the white dwarf, and likely corresponding to the emission of a dusty disc around the star. The finding of Ca, Fe and Mg absorption lines in two X-SHOOTER spectra of the white dwarf, taken 8 years apart, is further evidence of accretion from a dusty disc. We do not report variability in the absorption lines between these two spectra. Fitting a blackbody model to the infrared excess gives a temperature of 910$\pm50$ K. We have estimated a total accretion flux from the spectroscopic metal lines of $|\dot{\rm M}| = 1.784 \times 10^{9}\, $g s$^{-1}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.05731v2-abstract-full').style.display = 'none'; document.getElementById('2012.05731v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in MNRAS. 11 pages, 10 figures, 6 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2005.13221">arXiv:2005.13221</a> <span> [<a href="https://arxiv.org/pdf/2005.13221">pdf</a>, <a href="https://arxiv.org/ps/2005.13221">ps</a>, <a href="https://arxiv.org/format/2005.13221">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Popular Physics">physics.pop-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202037597">10.1051/0004-6361/202037597 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Qualitative classification of extraterrestrial civilizations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ivanov%2C+V+D">Valentin D. Ivanov</a>, <a href="/search/astro-ph?searchtype=author&query=Beamin%2C+J+C">Juan Carlos Beamin</a>, <a href="/search/astro-ph?searchtype=author&query=Caceres%2C+C">Claudio Caceres</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="2005.13221v2-abstract-short" style="display: inline;"> Abridged: The interest towards searches for extraterrestrial civilizations (ETCs) was boosted by the discovery of thousands of exoplanets. We turn to the classification of ETCs for new considerations that may help to design better strategies for ETCs searches. We take a basic taxonomic approach to ETCs and investigate the implications of the new classification on ETCs observational patterns. We us… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.13221v2-abstract-full').style.display = 'inline'; document.getElementById('2005.13221v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2005.13221v2-abstract-full" style="display: none;"> Abridged: The interest towards searches for extraterrestrial civilizations (ETCs) was boosted by the discovery of thousands of exoplanets. We turn to the classification of ETCs for new considerations that may help to design better strategies for ETCs searches. We take a basic taxonomic approach to ETCs and investigate the implications of the new classification on ETCs observational patterns. We use as a counter-example to our qualitative classification the quantitative scheme of Kardashev. We propose a classification based on the abilities of ETCs to modify their environment and to integrate with it: Class 0 uses the environment as it is, Class 1 modifies the it to fit its needs, Class 2 modifies itself to fit the environment and Class 3 ETC is fully integrated with the environment. Combined with the classical Kardashev's scale our scheme forms a 2d scheme for interpreting ETC properties. The new framework makes it obvious that the available energy is not an unique measure of ETCs, it may not even correlate with how well that energy is used. The possibility for progress without increased energy consumption implies lower detectability, so the existence of a Kardashev Type III ETC in the Milky Way cannot be ruled out. This reasoning weakens the Fermi paradox, allowing the existence of advanced, yet not energy hungry, low detectability ETCs. The integration of ETCs with environment makes it impossible to tell apart technosignatures from natural phenomena. Thus, the most likely opportunity for SETI searches is to look for beacons, specifically set up by them for young civilizations like us (if they want to do that is a matter of speculation). The other SETI window is to search for ETCs at technological level close to ours. To rephrase the saying of A. Clarke, sufficiently advanced civilizations are indistinguishable from nature. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.13221v2-abstract-full').style.display = 'none'; document.getElementById('2005.13221v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 May, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 May, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted in A&A; 7 pages, 1 figure; the acknowledgements were updated in the new version</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2005.05404">arXiv:2005.05404</a> <span> [<a href="https://arxiv.org/pdf/2005.05404">pdf</a>, <a href="https://arxiv.org/format/2005.05404">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/staa1352">10.1093/mnras/staa1352 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The VVV Infrared Variability Catalog (VIVA-I) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lopes%2C+C+E+F">C. E. Ferreira Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Cross%2C+N+J+G">N. J. G. Cross</a>, <a href="/search/astro-ph?searchtype=author&query=Catelan%2C+M">M. Catelan</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Hempel%2C+M">M. Hempel</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+P+W">P. W. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=Angeloni%2C+R">R. Angeloni</a>, <a href="/search/astro-ph?searchtype=author&query=Jablonsky%2C+F">F. Jablonsky</a>, <a href="/search/astro-ph?searchtype=author&query=Braga%2C+V+F">V. F. Braga</a>, <a href="/search/astro-ph?searchtype=author&query=Leao%2C+I+C">I. C. Leao</a>, <a href="/search/astro-ph?searchtype=author&query=Herpich%2C+F+R">F. R. Herpich</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=Papageorgiou%2C+A">A. Papageorgiou</a>, <a href="/search/astro-ph?searchtype=author&query=Pichara%2C+K">K. Pichara</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=Bradley%2C+A">A. Bradley</a>, <a href="/search/astro-ph?searchtype=author&query=Beamin%2C+J+C">J. C. Beamin</a>, <a href="/search/astro-ph?searchtype=author&query=Cortes%2C+C">C. Cortes</a>, <a href="/search/astro-ph?searchtype=author&query=De+Medeiros%2C+J+R">J. R. De Medeiros</a>, <a href="/search/astro-ph?searchtype=author&query=Russell%2C+C+M+P">Christopher. M. P. Russell</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="2005.05404v1-abstract-short" style="display: inline;"> Thanks to the VISTA Variables in the Via Lactea (VVV) ESO Public Survey it is now possible to explore a large number of objects in those regions. This paper addresses the variability analysis of all VVV point sources having more than 10 observations in VVVDR4 using a novel approach. In total, the near-IR light curves of 288,378,769 sources were analysed using methods developed in the New Insight I… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.05404v1-abstract-full').style.display = 'inline'; document.getElementById('2005.05404v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2005.05404v1-abstract-full" style="display: none;"> Thanks to the VISTA Variables in the Via Lactea (VVV) ESO Public Survey it is now possible to explore a large number of objects in those regions. This paper addresses the variability analysis of all VVV point sources having more than 10 observations in VVVDR4 using a novel approach. In total, the near-IR light curves of 288,378,769 sources were analysed using methods developed in the New Insight Into Time Series Analysis project. As a result, we present a complete sample having 44, 998, 752 variable star candidates (VVV-CVSC), which include accurate individual coordinates, near-IR magnitudes (ZYJHKs), extinctions A(Ks), variability indices, periods, amplitudes, among other parameters to assess the science. Unfortunately, a side effect of having a highly complete sample, is also having a high level of contamination by non-variable (contamination ratio of non-variables to variables is slightly over 10:1). To deal with this, we also provide some flags and parameters that can be used by the community to de-crease the number of variable candidates without heavily decreasing the completeness of the sample. In particular, we cross-identified 339,601 of our sources with Simbad and AAVSO databases, which provide us with information for these objects at other wavelegths. This sub-sample constitutes a unique resource to study the corresponding near-IR variability of known sources as well as to assess the IR variability related with X-ray and Gamma-Ray sources. On the other hand, the other 99.5% sources in our sample constitutes a number of potentially new objects with variability information for the heavily crowded and reddened regions of the Galactic Plane and Bulge. The present results also provide an important queryable resource to perform variability analysis and to characterize ongoing and future surveys like TESS and LSST. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.05404v1-abstract-full').style.display = 'none'; document.getElementById('2005.05404v1-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 May, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">27 pages, 14 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1908.10378">arXiv:1908.10378</a> <span> [<a href="https://arxiv.org/pdf/1908.10378">pdf</a>, <a href="https://arxiv.org/format/1908.10378">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="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201935998">10.1051/0004-6361/201935998 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Dust production in the debris disk around HR 4796 A </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Olofsson%2C+J">J. Olofsson</a>, <a href="/search/astro-ph?searchtype=author&query=Milli%2C+J">J. Milli</a>, <a href="/search/astro-ph?searchtype=author&query=Th%C3%A9bault%2C+P">P. Th茅bault</a>, <a href="/search/astro-ph?searchtype=author&query=Kral%2C+Q">Q. Kral</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%A9nard%2C+F">F. M茅nard</a>, <a href="/search/astro-ph?searchtype=author&query=Janson%2C+M">M. Janson</a>, <a href="/search/astro-ph?searchtype=author&query=Augereau%2C+J+-">J. -C. Augereau</a>, <a href="/search/astro-ph?searchtype=author&query=Bayo%2C+A">A. Bayo</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=Henning%2C+T">Th. Henning</a>, <a href="/search/astro-ph?searchtype=author&query=Iglesias%2C+D">D. Iglesias</a>, <a href="/search/astro-ph?searchtype=author&query=Kennedy%2C+G+M">G. M. Kennedy</a>, <a href="/search/astro-ph?searchtype=author&query=Montesinos%2C+M">M. Montesinos</a>, <a href="/search/astro-ph?searchtype=author&query=Pawellek%2C+N">N. Pawellek</a>, <a href="/search/astro-ph?searchtype=author&query=Schreiber%2C+M+R">M. R. Schreiber</a>, <a href="/search/astro-ph?searchtype=author&query=Zamora%2C+C">C. Zamora</a>, <a href="/search/astro-ph?searchtype=author&query=Carbillet%2C+M">M. Carbillet</a>, <a href="/search/astro-ph?searchtype=author&query=Feautrier%2C+P">P. Feautrier</a>, <a href="/search/astro-ph?searchtype=author&query=Fusco%2C+T">T. Fusco</a>, <a href="/search/astro-ph?searchtype=author&query=Madec%2C+F">F. Madec</a>, <a href="/search/astro-ph?searchtype=author&query=Rabou%2C+P">P. Rabou</a>, <a href="/search/astro-ph?searchtype=author&query=Sevin%2C+A">A. Sevin</a>, <a href="/search/astro-ph?searchtype=author&query=Szul%C3%A1gyi%2C+J">J. Szul谩gyi</a>, <a href="/search/astro-ph?searchtype=author&query=Zurlo%2C+A">A. Zurlo</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1908.10378v1-abstract-short" style="display: inline;"> Debris disks are the natural by-products of the planet formation process. Scattered or polarized light observations are mostly sensitive to small dust grains that are released from the grinding down of bigger planetesimals. High angular resolution observations at optical wavelengths can provide key constraints on the radial and azimuthal distribution of the small dust grains. These constraints can… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.10378v1-abstract-full').style.display = 'inline'; document.getElementById('1908.10378v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1908.10378v1-abstract-full" style="display: none;"> Debris disks are the natural by-products of the planet formation process. Scattered or polarized light observations are mostly sensitive to small dust grains that are released from the grinding down of bigger planetesimals. High angular resolution observations at optical wavelengths can provide key constraints on the radial and azimuthal distribution of the small dust grains. These constraints can help us better understand where most of the dust grains are released upon collisions. We present SPHERE/ZIMPOL observations of the debris disk around HR 4796 A, and model the radial profiles along several azimuthal angles of the disk with a code that accounts for the effect of stellar radiation pressure. This enables us to derive an appropriate description for the radial and azimuthal distribution of the small dust grains. Even though we only model the radial profiles along (or close to) the semi-major axis of the disk, our best-fit model is not only in good agreement with our observations but also with previously published datasets (from near-IR to sub-mm wavelengths). We find that the reference radius is located at $76.4\pm0.4$ au, and the disk has an eccentricity of $0.076_{-0.010}^{+0.016}$, with the pericenter located on the front side of the disk (north of the star). We find that small dust grains must be preferentially released near the pericenter to explain the observed brightness asymmetry. Even though parent bodies spend more time near the apocenter, the brightness asymmetry implies that collisions happen more frequently near the pericenter of the disk. Our model can successfully reproduce the shape of the outer edge of the disk, without having to invoke an outer planet shepherding the debris disk. With a simple treatment of the effect of the radiation pressure, we conclude that the parent planetesimals are located in a narrow ring of about $3.6$ au in width. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.10378v1-abstract-full').style.display = 'none'; document.getElementById('1908.10378v1-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, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 10 figures, accepted by 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 630, A142 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1902.07571">arXiv:1902.07571</a> <span> [<a href="https://arxiv.org/pdf/1902.07571">pdf</a>, <a href="https://arxiv.org/ps/1902.07571">ps</a>, <a href="https://arxiv.org/format/1902.07571">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/stz678">10.1093/mnras/stz678 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gaia Ultra-Cool Dwarf Sample -- II: Structure at the end of the main sequence </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Smart%2C+R+L">R. L. Smart</a>, <a href="/search/astro-ph?searchtype=author&query=Marocco%2C+F">F. Marocco</a>, <a href="/search/astro-ph?searchtype=author&query=Sarro%2C+L+M">L. M. Sarro</a>, <a href="/search/astro-ph?searchtype=author&query=Barrado%2C+D">D. Barrado</a>, <a href="/search/astro-ph?searchtype=author&query=Beamin%2C+J+C">J. C. Beamin</a>, <a href="/search/astro-ph?searchtype=author&query=Caballero%2C+J+A">J. A. Caballero</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+H+R+A">H. R. A. Jones</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1902.07571v1-abstract-short" style="display: inline;"> We identify and investigate known late M, L and T dwarfs in the Gaia second data release. This sample is being used as a training set in the Gaia data processing chain of the ultra cool dwarfs work package. We find 695 objects in the optical spectral range M8 to T6 with accurate Gaia coordinates, proper motions, and parallaxes which we combine with published spectral types and photometry from larg… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.07571v1-abstract-full').style.display = 'inline'; document.getElementById('1902.07571v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1902.07571v1-abstract-full" style="display: none;"> We identify and investigate known late M, L and T dwarfs in the Gaia second data release. This sample is being used as a training set in the Gaia data processing chain of the ultra cool dwarfs work package. We find 695 objects in the optical spectral range M8 to T6 with accurate Gaia coordinates, proper motions, and parallaxes which we combine with published spectral types and photometry from large area optical and infrared sky surveys. We find that 100 objects are in 47 multiple systems, of which 27 systems are published and 20 are new. These will be useful benchmark systems and we discuss the requirements to produce a complete catalog of multiple systems with an ultra cool dwarf component. We examine the magnitudes in the Gaia passbands and find that the GBP magnitudes are unreliable and should not be used for these objects. We examine progressively redder colour magnitude diagrams and see a notable increase in the main sequence scatter and a bivariate main sequence for old and young objects. We provide an absolute magnitude spectral sub-type calibration for G and GRP passbands along with linear fits over the range M8 L8 for other passbands. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.07571v1-abstract-full').style.display = 'none'; document.getElementById('1902.07571v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 February, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 24 figures, submitted to MNRAS but still time to make minor changes</span> </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/1806.09252">arXiv:1806.09252</a> <span> [<a href="https://arxiv.org/pdf/1806.09252">pdf</a>, <a href="https://arxiv.org/format/1806.09252">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="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stz1133">10.1093/mnras/stz1133 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Sub-millimeter non-contaminated detection of the disk around TWA\,7 by ALMA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bayo%2C+A">A. Bayo</a>, <a href="/search/astro-ph?searchtype=author&query=Olofsson%2C+J">J. Olofsson</a>, <a href="/search/astro-ph?searchtype=author&query=Matra%2C+L">L. Matra</a>, <a href="/search/astro-ph?searchtype=author&query=Beamin%2C+J+C">J. C. Beamin</a>, <a href="/search/astro-ph?searchtype=author&query=Gallardo%2C+J">J. Gallardo</a>, <a href="/search/astro-ph?searchtype=author&query=de+Gregorio-Monsalvo%2C+I">I. de Gregorio-Monsalvo</a>, <a href="/search/astro-ph?searchtype=author&query=Booth%2C+M">M. Booth</a>, <a href="/search/astro-ph?searchtype=author&query=Zamora%2C+C">C. Zamora</a>, <a href="/search/astro-ph?searchtype=author&query=Iglesias%2C+D">D. Iglesias</a>, <a href="/search/astro-ph?searchtype=author&query=Henning%2C+T">Th. Henning</a>, <a href="/search/astro-ph?searchtype=author&query=Schreiber%2C+M+R">M. R. Schreiber</a>, <a href="/search/astro-ph?searchtype=author&query=Caceres%2C+C">C. Caceres</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1806.09252v3-abstract-short" style="display: inline;"> Debris disks can be seen as the left-overs of giant planet formation and the possible nurseries of rocky planets. While M-type stars out-number more massive stars we know very little about the time evolution of their circumstellar disks at ages older than $\sim 10$\,Myr. Sub-millimeter observations are best to provide first order estimates of the available mass reservoir and thus better constrain… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.09252v3-abstract-full').style.display = 'inline'; document.getElementById('1806.09252v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1806.09252v3-abstract-full" style="display: none;"> Debris disks can be seen as the left-overs of giant planet formation and the possible nurseries of rocky planets. While M-type stars out-number more massive stars we know very little about the time evolution of their circumstellar disks at ages older than $\sim 10$\,Myr. Sub-millimeter observations are best to provide first order estimates of the available mass reservoir and thus better constrain the evolution of such disks. Here, we present ALMA Cycle\,3 Band\,7 observations of the debris disk around the M2 star TWA\,7, which had been postulated to harbor two spatially separated dust belts, based on unresolved far-infrared and sub-millimeter data. We show that most of the emission at wavelengths longer than $\sim 300$\,$渭$m is in fact arising from a contaminant source, most likely a sub-mm galaxy, located at about 6.6" East of TWA\,7 (in 2016). Fortunately, the high resolution of our ALMA data allows us to disentangle the contaminant emission from that of the disc and report a significant detection of the disk in the sub-millimeter for the first time with a flux density of 2.1$\pm$0.4 mJy at 870 $渭$m. With this detection, we show that the SED can be reproduced with a single dust belt. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.09252v3-abstract-full').style.display = 'none'; document.getElementById('1806.09252v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 June, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">6 pages, accepted to 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/1712.00041">arXiv:1712.00041</a> <span> [<a href="https://arxiv.org/pdf/1712.00041">pdf</a>, <a href="https://arxiv.org/format/1712.00041">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/aa9ee2">10.3847/1538-3881/aa9ee2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Searching for Extragalactic Sources in the VISTA Variables in the V铆a L谩ctea Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Baravalle%2C+L+D">Laura D. Baravalle</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso%2C+M+V">M. Victoria Alonso</a>, <a href="/search/astro-ph?searchtype=author&query=Castell%C3%B3n%2C+J+L+N">Jos茅 L. Nilo Castell贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Beam%C3%ADn%2C+J+C">Juan C. Beam铆n</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="1712.00041v1-abstract-short" style="display: inline;"> We search for extragalactic sources in the VISTA Variables in the V铆a L谩ctea survey that are hidden by the Galaxy. Herein, we describe our photometric procedure to find and characterize extragalactic objects using a combination of SExtractor and PSFEx. It was applied in two tiles of the survey: d010 and d115, without previous extragalactic IR detections, in order to obtain photometric parameters o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1712.00041v1-abstract-full').style.display = 'inline'; document.getElementById('1712.00041v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1712.00041v1-abstract-full" style="display: none;"> We search for extragalactic sources in the VISTA Variables in the V铆a L谩ctea survey that are hidden by the Galaxy. Herein, we describe our photometric procedure to find and characterize extragalactic objects using a combination of SExtractor and PSFEx. It was applied in two tiles of the survey: d010 and d115, without previous extragalactic IR detections, in order to obtain photometric parameters of the detected sources. The adopted criteria to define extragalactic candidates include CLASS_STAR < 0.3; 1.0 < R1/2 < 5.0 arcsec; 2.1 < C < 5; and Phi > 0.002 and the colors: 0.5 < (J - K_s) < 2.0 mag; 0.0 < (J - H) < 1.0 mag; 0.0 < (H - K_s) < 2.0 mag and (J - H) + 0.9 (H - K_s) > 0.44 mag. We detected 345 and 185 extragalactic candidates in the d010 and d115 tiles, respectively. All of them were visually inspected and confirmed to be galaxies. In general, they are small and more circular objects, due to the near-IR sensitivity to select more compact objects with higher surface brightness. The procedure will be used to identify extragalactic objects in other tiles of the VVV disk, which will allow us to study the distribution of galaxies and filaments hidden by the Milky Way. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1712.00041v1-abstract-full').style.display = 'none'; document.getElementById('1712.00041v1-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 November, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">25 pages, 2 tables, 15 figures. Accepted for publication in The Astronomical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1708.05365">arXiv:1708.05365</a> <span> [<a href="https://arxiv.org/pdf/1708.05365">pdf</a>, <a href="https://arxiv.org/format/1708.05365">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="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stx2144">10.1093/mnras/stx2144 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Searching for Faint Comoving Companions to the $伪$ Centauri system in the VVV Survey Infrared Images </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Beamin%2C+J+C">J. C. Beamin</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</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=Ivanov%2C+V+D">V. D. Ivanov</a>, <a href="/search/astro-ph?searchtype=author&query=Bendek%2C+E">E. Bendek</a>, <a href="/search/astro-ph?searchtype=author&query=Bayo%2C+A">A. Bayo</a>, <a href="/search/astro-ph?searchtype=author&query=Gromadzki%2C+M">M. Gromadzki</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtev%2C+R">R. Kurtev</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+P+W">P. W. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=Butler%2C+R+P">R. P. Butler</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="1708.05365v1-abstract-short" style="display: inline;"> The VVV survey has observed the southern disk of the Milky Way in the near infrared, covering 240 deg$^{2}$ in the $ZYJHK_S$ filters. We search the VVV Survey images in a $\sim$19 deg$^{2}$ field around $伪$ Centauri, the nearest stellar system to the Sun, to look for possible overlooked companions that the baseline in time of VVV would be able to uncover. The photometric depth of our search reache… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1708.05365v1-abstract-full').style.display = 'inline'; document.getElementById('1708.05365v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1708.05365v1-abstract-full" style="display: none;"> The VVV survey has observed the southern disk of the Milky Way in the near infrared, covering 240 deg$^{2}$ in the $ZYJHK_S$ filters. We search the VVV Survey images in a $\sim$19 deg$^{2}$ field around $伪$ Centauri, the nearest stellar system to the Sun, to look for possible overlooked companions that the baseline in time of VVV would be able to uncover. The photometric depth of our search reaches $Y\sim$19.3 mag, $J\sim$19 mag, and $K_S\sim$17 mag. This search has yielded no new companions in $伪$ Centauri system, setting an upper mass limit for any unseen companion well into the brown dwarf/planetary mass regime. The apparent magnitude limits were turned into effective temperature limits, and the presence of companion objects with effective temperatures warmer than 325K can be ruled out using different state-of-the-art atmospheric models. These limits were transformed into mass limits using evolutionary models, companions with masses above 11 M$_{Jup}$ were discarded, extending the constraints recently provided in the literature up to projected distances of d<7 000 AU from $伪$ Cen AB and $\sim$1200 AU from Proxima. In the next few years, the VVV extended survey (VVVX) will allow to extend the search and place similar limits on brown dwarfs/planetary companions to $伪$ Cen AB for separations up to 20 000AU. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1708.05365v1-abstract-full').style.display = 'none'; document.getElementById('1708.05365v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 August, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">8 pages, 6 figures, 3 tables. Accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1703.09454">arXiv:1703.09454</a> <span> [<a href="https://arxiv.org/pdf/1703.09454">pdf</a>, <a href="https://arxiv.org/ps/1703.09454">ps</a>, <a href="https://arxiv.org/format/1703.09454">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stx800">10.1093/mnras/stx800 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gaia Ultracool Dwarf Sample. I. Known L and T dwarfs and the first Gaia data release </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Smart%2C+R+L">R. L. Smart</a>, <a href="/search/astro-ph?searchtype=author&query=Marocco%2C+F">F. Marocco</a>, <a href="/search/astro-ph?searchtype=author&query=Caballero%2C+J+A">J. A. Caballero</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+H+R+A">H. R. A. Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Barrado%2C+D">D. Barrado</a>, <a href="/search/astro-ph?searchtype=author&query=Beamin%2C+J+C">J. C. Beamin</a>, <a href="/search/astro-ph?searchtype=author&query=Pinfield%2C+D+J">D. J. Pinfield</a>, <a href="/search/astro-ph?searchtype=author&query=Sarro%2C+L+M">L. M. Sarro</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1703.09454v1-abstract-short" style="display: inline;"> We identify and investigate known ultracool stars and brown dwarfs that are being observed or indirectly constrained by the Gaia mission. These objects will be the core of the Gaia ultracool dwarf sample composed of all dwarfs later than M7 that Gaia will provide direct or indirect information on. We match known L and T dwarfs to the Gaia first data release, the Two Micron All Sky Survey and the W… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.09454v1-abstract-full').style.display = 'inline'; document.getElementById('1703.09454v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1703.09454v1-abstract-full" style="display: none;"> We identify and investigate known ultracool stars and brown dwarfs that are being observed or indirectly constrained by the Gaia mission. These objects will be the core of the Gaia ultracool dwarf sample composed of all dwarfs later than M7 that Gaia will provide direct or indirect information on. We match known L and T dwarfs to the Gaia first data release, the Two Micron All Sky Survey and the Wide-field Infrared Survey Explorer AllWISE survey and examine the Gaia and infrared colours, along with proper motions, to improve spectral typing, identify outliers and find mismatches. There are 321 L and T dwarfs observed directly in the Gaia first data release, of which 10 are later than L7. This represents 45 % of all the known LT dwarfs with estimated Gaia G magnitudes brighter than 20.3 mag. We determine proper motions for the 321 objects from Gaia and the Two Micron All Sky Survey positions. Combining the Gaia and infrared magnitudes provides useful diagnostic diagrams for the determination of L and T dwarf physical parameters. We then search the Tycho-Gaia astrometric solution Gaia first data release subset to find any objects with common proper motions to known L and T dwarfs and a high probability of being related. We find 15 new candidate common proper motion systems. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.09454v1-abstract-full').style.display = 'none'; document.getElementById('1703.09454v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 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">Accepted by MNRAS, 17 pages, appendix of 6 pages, two online tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1703.05817">arXiv:1703.05817</a> <span> [<a href="https://arxiv.org/pdf/1703.05817">pdf</a>, <a href="https://arxiv.org/ps/1703.05817">ps</a>, <a href="https://arxiv.org/format/1703.05817">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Near-IR trigonometric parallaxes of nearby stars in the Galactic plane using the VVV </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Beamin%2C+J+C">J. C. Beamin</a>, <a href="/search/astro-ph?searchtype=author&query=Mendez%2C+R+A">R. A. Mendez</a>, <a href="/search/astro-ph?searchtype=author&query=Smart%2C+R+L">R. L. Smart</a>, <a href="/search/astro-ph?searchtype=author&query=Jara%2C+R">R. Jara</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtev%2C+R">R. Kurtev</a>, <a href="/search/astro-ph?searchtype=author&query=Gromadzki%2C+M">M. Gromadzki</a>, <a href="/search/astro-ph?searchtype=author&query=Villanueva%2C+V">V. Villanueva</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</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=Lucas%2C+P+W">P. W. Lucas</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1703.05817v1-abstract-short" style="display: inline;"> We use the multi-epoch K$\rm _S$ band observations, covering a $\sim$5 years baseline to obtain milli and sub-milli arcsec precision astrometry for a sample of eighteen previously known high proper motion sources, including precise parallaxes for these sources for the first time. In this study we show the capability of the VVV project to measure high precision trigonometric parallaxes for very low… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.05817v1-abstract-full').style.display = 'inline'; document.getElementById('1703.05817v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1703.05817v1-abstract-full" style="display: none;"> We use the multi-epoch K$\rm _S$ band observations, covering a $\sim$5 years baseline to obtain milli and sub-milli arcsec precision astrometry for a sample of eighteen previously known high proper motion sources, including precise parallaxes for these sources for the first time. In this study we show the capability of the VVV project to measure high precision trigonometric parallaxes for very low mass stars (VLMS) up to distances of $\sim$250\,pc reaching farther than most other ground based surveys or space missions for these types of stars. Additionally, we used spectral energy distribution to search for evidence of unresolved binary systems and cool sub-dwarfs. We detected five systems that are most likely VLMS belonging to the Galactic halo based on their tangential velocities, and four objects within 60 pc that are likely members of the thick disk. A more comprehensive study of high proper motion sources and parallaxes of VLMS and brown dwarfs with the VVV is ongoing , including thousands of newly discovered objects. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.05817v1-abstract-full').style.display = 'none'; document.getElementById('1703.05817v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 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">4 pages, 1 table, 2 figures. Proceedings of the VII ADELA (Bogota, Colombia) and XV LARIM (Cartagena de Indias, Colombia) conferences</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1610.06951">arXiv:1610.06951</a> <span> [<a href="https://arxiv.org/pdf/1610.06951">pdf</a>, <a href="https://arxiv.org/format/1610.06951">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/stw2760">10.1093/mnras/stw2760 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Physical parameters of late M-type members of Chamaleon I and TW Hydrae Association: Dust settling, age dispersion and activity </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bayo%2C+A">A. Bayo</a>, <a href="/search/astro-ph?searchtype=author&query=Barrado%2C+D">D. Barrado</a>, <a href="/search/astro-ph?searchtype=author&query=Allard%2C+F">F. Allard</a>, <a href="/search/astro-ph?searchtype=author&query=Henning%2C+T">T. Henning</a>, <a href="/search/astro-ph?searchtype=author&query=Comeron%2C+F">F. Comeron</a>, <a href="/search/astro-ph?searchtype=author&query=Morales-Calderon%2C+M">M. Morales-Calderon</a>, <a href="/search/astro-ph?searchtype=author&query=Rajpurohit%2C+A+S">A. S. Rajpurohit</a>, <a href="/search/astro-ph?searchtype=author&query=Ram%C4%B1rez%2C+K+P">K. Pena Ram谋rez</a>, <a href="/search/astro-ph?searchtype=author&query=Beam%C4%B1n%2C+J+C">J. C. Beam谋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="1610.06951v1-abstract-short" style="display: inline;"> Although mid-to-late type M dwarfs are the most common stars in our stellar neighborhood, our knowledge of these objects is still limited. Open questions include the evolution of their angular momentum, internal structures, dust settling in their atmospheres, age dispersion within populations. In addition, at young ages, late-type Ms have masses below the hydrogen burning limit and therefore are k… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1610.06951v1-abstract-full').style.display = 'inline'; document.getElementById('1610.06951v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1610.06951v1-abstract-full" style="display: none;"> Although mid-to-late type M dwarfs are the most common stars in our stellar neighborhood, our knowledge of these objects is still limited. Open questions include the evolution of their angular momentum, internal structures, dust settling in their atmospheres, age dispersion within populations. In addition, at young ages, late-type Ms have masses below the hydrogen burning limit and therefore are key objects in the debate on the brown dwarf mechanism of formation. In this work we determine and study in detail the physical parameters of two samples of young, late M-type sources belonging to either the Chamaeleon I Dark Cloud or the TW Hydrae Association and compare them with the results obtained in the literature for other young clusters and also for older, field, dwarfs. We used multi-wavelength photometry to construct and analyze SEDs to determine general properties of the photosphere and disk presence. We also used low resolution optical and near-infrared spectroscopy to study activity, accretion, gravity and effective temperature sensitive indicators. We propose a VO-based spectral index that is both temperature and age sensitive. We derived physical parameters using independent techniques confirming the already common feature/problem of the age/luminosity spread. In particular, we highlight two brown dwarfs showing very similar temperatures but clearly different surface gravity (explained invoking extreme early accretion). We also show how, despite large improvement in the dust treatment in theoretical models, there is still room for further progress in the simultaneous reproduction of the optical and near-infrared features of these cold young objects. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1610.06951v1-abstract-full').style.display = 'none'; document.getElementById('1610.06951v1-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 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">26 pages, 22 figures, 10 tables. Accepted in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1609.03520">arXiv:1609.03520</a> <span> [<a href="https://arxiv.org/pdf/1609.03520">pdf</a>, <a href="https://arxiv.org/ps/1609.03520">ps</a>, <a href="https://arxiv.org/format/1609.03520">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/stw2357">10.1093/mnras/stw2357 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> VVV High proper motion stars I. The catalogue of bright Ks < 13.5 stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kurtev%2C+R">R. Kurtev</a>, <a href="/search/astro-ph?searchtype=author&query=Gromadzki%2C+M">M. Gromadzki</a>, <a href="/search/astro-ph?searchtype=author&query=Beamin%2C+J+C">J. C. Beamin</a>, <a href="/search/astro-ph?searchtype=author&query=Folkes%2C+S+L">S. L. Folkes</a>, <a href="/search/astro-ph?searchtype=author&query=Ramirez%2C+K+P">K. Pena Ramirez</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=Borissova%2C+J">J. Borissova</a>, <a href="/search/astro-ph?searchtype=author&query=Villanueva%2C+V">V. Villanueva</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Mendez%2C+R">R. Mendez</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=Smith%2C+L+C">L. C. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Pinfield%2C+D+J">D. J. Pinfield</a>, <a href="/search/astro-ph?searchtype=author&query=Kuhn%2C+M+A">M. A. Kuhn</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+H+R+A">H. R. A. Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Antonova%2C+A">A. Antonova</a>, <a href="/search/astro-ph?searchtype=author&query=Yip%2C+A+K+P">A. K. P. Yip</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1609.03520v1-abstract-short" style="display: inline;"> Knowledge of the stellar content near the Sun is important for a broad range of topics ranging from the search for planets to the study of Milky Way structure. The most powerful method for identifying potentially nearby stars is proper motion (PM) surveys. All old optical surveys avoid, or are at least substantially incomplete, near the Galactic plane. The depth and breadth of the "Vista Variables… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.03520v1-abstract-full').style.display = 'inline'; document.getElementById('1609.03520v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1609.03520v1-abstract-full" style="display: none;"> Knowledge of the stellar content near the Sun is important for a broad range of topics ranging from the search for planets to the study of Milky Way structure. The most powerful method for identifying potentially nearby stars is proper motion (PM) surveys. All old optical surveys avoid, or are at least substantially incomplete, near the Galactic plane. The depth and breadth of the "Vista Variables in Via Lactea" (VVV) near-IR survey significantly improves this situation. Taking advantage of the VVV survey database, we have measured PMs in the densest regions of the MW bulge and southern plane in order to complete the census of nearby objects. We have developed a custom PM pipeline based on VVV catalogues from the Cambridge Astronomy Survey Unit (CASU), by comparing the first epoch of JHKs with the multi-epoch Ks-bands acquired later. Taking advantage of the large time baseline between the 2MASS and the VVV observations, we also obtained 2MASS-VVV PMs. We present a near-IR proper motion catalogue for the whole area of the VVV survey, which includes 3003 moving stellar sources. All of these have been visually inspected and are real PM objects. Our catalogue is in very good agreement with the proper motion data supplied in IR catalogues outside the densest zone of the MW. The majority of the PM objects in our catalogue are nearby M-dwarfs, as expected. This new database allow us to identify 57 common proper motion binary candidates, among which are two new systems within ~30pc of the Sun. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.03520v1-abstract-full').style.display = 'none'; document.getElementById('1609.03520v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 September, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 7 figures, accepted in the MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1609.02796">arXiv:1609.02796</a> <span> [<a href="https://arxiv.org/pdf/1609.02796">pdf</a>, <a href="https://arxiv.org/ps/1609.02796">ps</a>, <a href="https://arxiv.org/format/1609.02796">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"> High proper motion objects towards the inner Milky Way: characterisation of newly identified nearby stars from the VISTA Variables in the Via Lactea Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gromadzki%2C+M">M. Gromadzki</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtev%2C+R">R. Kurtev</a>, <a href="/search/astro-ph?searchtype=author&query=Beamin%2C+J+C">J. C. Beamin</a>, <a href="/search/astro-ph?searchtype=author&query=Tekola%2C+A">A. Tekola</a>, <a href="/search/astro-ph?searchtype=author&query=Ramphul%2C+R">R. Ramphul</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=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Folkes%2C+S+L">S. L. Folkes</a>, <a href="/search/astro-ph?searchtype=author&query=Vaisanen%2C+P">P. Vaisanen</a>, <a href="/search/astro-ph?searchtype=author&query=Kniazev%2C+A+Y">A. Y. Kniazev</a>, <a href="/search/astro-ph?searchtype=author&query=Borissova%2C+J">J. Borissova</a>, <a href="/search/astro-ph?searchtype=author&query=Parsons%2C+S+G">S. G. Parsons</a>, <a href="/search/astro-ph?searchtype=author&query=Villanueva%2C+V">V. Villanueva</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1609.02796v2-abstract-short" style="display: inline;"> The census of the Solar neighbourhood is still incomplete, as demonstrated by recent discoveries of many objects within 5-10 pc from the Sun. The area around the mid-plane and bulge of the Milky Way presents the most difficulties in searches for such nearby objects, and is therefore deficient in the known population. This is largely due to high stellar densities encountered. Spectroscopic, photome… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.02796v2-abstract-full').style.display = 'inline'; document.getElementById('1609.02796v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1609.02796v2-abstract-full" style="display: none;"> The census of the Solar neighbourhood is still incomplete, as demonstrated by recent discoveries of many objects within 5-10 pc from the Sun. The area around the mid-plane and bulge of the Milky Way presents the most difficulties in searches for such nearby objects, and is therefore deficient in the known population. This is largely due to high stellar densities encountered. Spectroscopic, photometric and kinematic characterization of these objects allows better understand the local mass function, the binary fraction, and provides new interesting targets for more detailed studies. We report the spectroscopic follow-up and characterisation of 12 bright high PM objects, identified from the VISTA Variables in Via Lactea survey (VVV). We used the 1.9-m telescope of the South African Astronomical Observatory (SAAO) for low-resolution optical spectroscopy and spectral classification, and the MPG/ESP 2.2m telescope Fiber-fed Extended Range Optical Spectrograph (FEROS) high-resolution optical spectroscopy to obtain the radial and space velocities for three of them. Six of our objects have co-moving companions. We derived optical spectral types and photometric distances, and classified all of them as K and M dwarfs within 27-264 pc of the Sun. Finally, we found that one of the sources, VVV J141421.23-602326.1 (a co-moving companion of VVV J141420.55-602337.1), appears to be a rare massive white dwarf that maybe close to the ZZ Ceti instability strip. Many of the objects in our list are interesting targets for exoplanet searches. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.02796v2-abstract-full').style.display = 'none'; document.getElementById('1609.02796v2-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, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 September, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 2 figures, accepted for publication in Acta Astronomica</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1605.08620">arXiv:1605.08620</a> <span> [<a href="https://arxiv.org/pdf/1605.08620">pdf</a>, <a href="https://arxiv.org/format/1605.08620">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201628662">10.1051/0004-6361/201628662 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Near-infrared photometry of WISE J085510.74$-$071442.5 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Osorio%2C+M+R+Z">M. R. Zapatero Osorio</a>, <a href="/search/astro-ph?searchtype=author&query=Lodieu%2C+N">N. Lodieu</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%A9jar%2C+V+J+S">V. J. S. B茅jar</a>, <a href="/search/astro-ph?searchtype=author&query=Mart%C3%ADn%2C+E+L">E. L. Mart铆n</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=Bayo%2C+A">A. Bayo</a>, <a href="/search/astro-ph?searchtype=author&query=Boffin%2C+H+M+J">H. M. J. Boffin</a>, <a href="/search/astro-ph?searchtype=author&query=Mu%C5%BEi%C4%87%2C+K">K. Mu啪i膰</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Beam%C3%ADn%2C+J+C">J. C. Beam铆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="1605.08620v1-abstract-short" style="display: inline;"> (Abridged) We aim at measuring the near-infrared photometry, and deriving the mass, age, temperature, and surface gravity of WISE J085510.74-071442.5 (J0855-0714), which is the coolest known object beyond the Solar System as of today. We use publicly available data from the archives of the HST and the VLT to determine the emission of this source at 1.153 micron (F110W) and 1.575 micron (CH_4). J08… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.08620v1-abstract-full').style.display = 'inline'; document.getElementById('1605.08620v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1605.08620v1-abstract-full" style="display: none;"> (Abridged) We aim at measuring the near-infrared photometry, and deriving the mass, age, temperature, and surface gravity of WISE J085510.74-071442.5 (J0855-0714), which is the coolest known object beyond the Solar System as of today. We use publicly available data from the archives of the HST and the VLT to determine the emission of this source at 1.153 micron (F110W) and 1.575 micron (CH_4). J0855-0714 is detected at both wavelengths with signal-to-noise ratio of ~10 (F110W) and ~4 (CH_4-off) at the peak of the corresponding PSFs. This is the first detection of J0855-0714 in the H-band. We measure 26.31 +/- 0.10 and 23.22 +/- 0.35 mag in F110W and CH_4 (Vega system). J0855-0714 remains unresolved in the HST images that have a spatial resolution of 0.22". Companions at separations of 0.5 AU (similar brightness) and at ~1 AU (~1 mag fainter in the F110W filter) are discarded. By combining the new data with published photometry, we build the spectral energy distribution of J0855-0714 from 0.89 to 22.09 micron, and contrast it against state-of-the-art solar-metallicity models of planetary atmospheres. We determine a temperature of 225-250 K, a bolometric luminosity of log L/Lsol = -8.57, and a high surface gravity of log g = 5.0 (cm/s2), which suggests an old age although such a high gravity is not fully compatible with evolutionary models. After comparison with the cooling theory for brown dwarfs and planets, we infer a mass in the interval 2-10 Mjup for ages of 1-12 Gyr and log g > 3.5 (cm/s2). At the age of the Sun, J0855-0714 would be a ~5-Mjup free-floating planetary-mass object. J0855-0714 may represent the old image of the free-floating planetary-mass objects of similar mass discovered in star-forming regions and young stellar clusters. As many J0855-0714-like objects as M5-L2 stars may be expected to populate the solar neighborhood. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.08620v1-abstract-full').style.display = 'none'; document.getElementById('1605.08620v1-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 May, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">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 592, A80 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1509.09226">arXiv:1509.09226</a> <span> [<a href="https://arxiv.org/pdf/1509.09226">pdf</a>, <a href="https://arxiv.org/ps/1509.09226">ps</a>, <a href="https://arxiv.org/format/1509.09226">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/stv2290">10.1093/mnras/stv2290 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery of a brown dwarf companion to the A3V star 尾 Circini </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Smith%2C+L+C">L. C. Smith</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=Pe%C3%B1a%2C+C+C">C. Contreras Pe帽a</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtev%2C+R">R. Kurtev</a>, <a href="/search/astro-ph?searchtype=author&query=Marocco%2C+F">F. Marocco</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+H+R+A">H. R. A. Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Beamin%2C+J+C">J. C. Beamin</a>, <a href="/search/astro-ph?searchtype=author&query=Napiwotzki%2C+R">R. Napiwotzki</a>, <a href="/search/astro-ph?searchtype=author&query=Borissova%2C+J">J. Borissova</a>, <a href="/search/astro-ph?searchtype=author&query=Burningham%2C+B">B. Burningham</a>, <a href="/search/astro-ph?searchtype=author&query=Faherty%2C+J">J. Faherty</a>, <a href="/search/astro-ph?searchtype=author&query=Pinfield%2C+D+J">D. J. Pinfield</a>, <a href="/search/astro-ph?searchtype=author&query=Gromadzki%2C+M">M. Gromadzki</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=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Stimson%2C+W">W. Stimson</a>, <a href="/search/astro-ph?searchtype=author&query=Villanueva%2C+V">V. Villanueva</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1509.09226v1-abstract-short" style="display: inline;"> We report the discovery of an L dwarf companion to the A3V star 尾 Circini. VVV J151721.49-585131.5, or 尾 Cir B, was identified in a proper motion and parallax catalogue of the Vista Variables in the V铆a L谩ctea survey as having near infrared luminosity and colour indicative of an early L dwarf, and a proper motion and parallax consistent with that of 尾 Cir. The projected separation of $\sim$3.6' co… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.09226v1-abstract-full').style.display = 'inline'; document.getElementById('1509.09226v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1509.09226v1-abstract-full" style="display: none;"> We report the discovery of an L dwarf companion to the A3V star 尾 Circini. VVV J151721.49-585131.5, or 尾 Cir B, was identified in a proper motion and parallax catalogue of the Vista Variables in the V铆a L谩ctea survey as having near infrared luminosity and colour indicative of an early L dwarf, and a proper motion and parallax consistent with that of 尾 Cir. The projected separation of $\sim$3.6' corresponds to $6656$ au, which is unusually wide. The most recent published estimate of the age of the primary combined with our own estimate based on newer isochrones yields an age of $370-500$ Myr. The system therefore serves as a useful benchmark at an age greater than that of the Pleiades brown dwarfs and most other young L dwarf benchmarks. We have obtained a medium resolution echelle spectrum of the companion which indicates a spectral type of L1.0$\pm$0.5 and lacks the typical signatures of low surface gravity seen in younger brown dwarfs. This suggests that signs of low surface gravity disappear from the spectra of early L dwarfs by an age of $\sim370-500$ Myr, as expected from theoretical isochrones. The mass of 尾 Cir B is estimated from the BHAC15 isochrones as $0.056\pm0.007$ M$_{\odot}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.09226v1-abstract-full').style.display = 'none'; document.getElementById('1509.09226v1-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 September, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in the MNRAS main journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1509.07507">arXiv:1509.07507</a> <span> [<a href="https://arxiv.org/pdf/1509.07507">pdf</a>, <a href="https://arxiv.org/ps/1509.07507">ps</a>, <a href="https://arxiv.org/format/1509.07507">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/stv2241">10.1093/mnras/stv2241 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Spectro-photometric characterization of high proper motion sources from WISE </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Ivanov%2C+V+D">V. D. Ivanov</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Smart%2C+R+L">R. L. Smart</a>, <a href="/search/astro-ph?searchtype=author&query=Muzic%2C+K">K. Muzic</a>, <a href="/search/astro-ph?searchtype=author&query=Mendez%2C+R+A">R. A. Mendez</a>, <a href="/search/astro-ph?searchtype=author&query=Beletsky%2C+Y">Y. Beletsky</a>, <a href="/search/astro-ph?searchtype=author&query=Bayo%2C+A">A. Bayo</a>, <a href="/search/astro-ph?searchtype=author&query=Gromadzki%2C+M">M. Gromadzki</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtev%2C+R">R. Kurtev</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1509.07507v1-abstract-short" style="display: inline;"> The census of the solar neighborhood is almost complete for stars and becoming more complete in the brown dwarf regime. Spectroscopic, photometric and kinematic characterization of nearby objects helps us to understand the local mass function, the binary fraction, and provides new targets for sensitive planet searches. We aim to derive spectral types and spectro-photometric distances of a sample o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.07507v1-abstract-full').style.display = 'inline'; document.getElementById('1509.07507v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1509.07507v1-abstract-full" style="display: none;"> The census of the solar neighborhood is almost complete for stars and becoming more complete in the brown dwarf regime. Spectroscopic, photometric and kinematic characterization of nearby objects helps us to understand the local mass function, the binary fraction, and provides new targets for sensitive planet searches. We aim to derive spectral types and spectro-photometric distances of a sample of new high proper motion sources found with the WISE satellite, and obtain parallaxes for those objects that fall within the area observed by the Vista Variables in the V铆a L谩ctea survey (VVV). We used low resolution spectroscopy and template fitting to derive spectral types, multiwavelength photometry to characterize the companion candidates and obtain photometric distances. Multi-epoch imaging from the VVV survey was used to measure the parallaxes and proper motions for three sources. We confirm a new T2 brown dwarf within $\sim$15 pc. We derived optical spectral types for twenty four sources, mostly M dwarfs within 50 pc. We addressed the wide binary nature of sixteen objects found by the WISE mission and previously known high proper motion sources. Six of these are probably members of wide binaries, two of those are new, and present evidence against the physical binary nature of two candidate binary stars found in the literature, and eight that we selected as possible binary systems. We discuss a likely microlensing event produced by a nearby low mass star and a galaxy, that is to occur in the following five years. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.07507v1-abstract-full').style.display = 'none'; document.getElementById('1509.07507v1-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 September, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 5 figures, 5 tables, accepted MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1410.6792">arXiv:1410.6792</a> <span> [<a href="https://arxiv.org/pdf/1410.6792">pdf</a>, <a href="https://arxiv.org/ps/1410.6792">ps</a>, <a href="https://arxiv.org/format/1410.6792">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/10.1051/0004-6361/201424883">10.1051/0004-6361/201424883 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Properties of the solar neighbor WISE J072003.20-084651.2 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ivanov%2C+V+D">V. D. Ivanov</a>, <a href="/search/astro-ph?searchtype=author&query=Vaisanen%2C+P">P. Vaisanen</a>, <a href="/search/astro-ph?searchtype=author&query=Kniazev%2C+A+Y">A. Y. Kniazev</a>, <a href="/search/astro-ph?searchtype=author&query=Beletsky%2C+Y">Y. Beletsky</a>, <a href="/search/astro-ph?searchtype=author&query=Mamajek%2C+E+E">E. E. Mamajek</a>, <a href="/search/astro-ph?searchtype=author&query=Muzic%2C+K">K. Muzic</a>, <a href="/search/astro-ph?searchtype=author&query=Beamin%2C+J+C">J. C. Beamin</a>, <a href="/search/astro-ph?searchtype=author&query=Boffin%2C+H+M+J">H. M. J. Boffin</a>, <a href="/search/astro-ph?searchtype=author&query=Pourbaix%2C+D">D. Pourbaix</a>, <a href="/search/astro-ph?searchtype=author&query=Gandhi%2C+P">P. Gandhi</a>, <a href="/search/astro-ph?searchtype=author&query=Gulbis%2C+A">A. Gulbis</a>, <a href="/search/astro-ph?searchtype=author&query=Monaco%2C+L">L. Monaco</a>, <a href="/search/astro-ph?searchtype=author&query=Saviane%2C+I">I. Saviane</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtev%2C+R">R. Kurtev</a>, <a href="/search/astro-ph?searchtype=author&query=Mawet%2C+D">D. Mawet</a>, <a href="/search/astro-ph?searchtype=author&query=Borissova%2C+J">J. Borissova</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1410.6792v1-abstract-short" style="display: inline;"> The severe crowding towards the Galactic plane suggests that the census of nearby stars in that direction may be incomplete. Recently, Scholz reported a new M9 object at an estimated distance d~7 pc (WISE J072003.20-084651.2; hereafter WISE0720) at Galactic latitude b=2.3 degr. Our goals are to determine the physical characteristics of WISE0720, its kinematic properties, and to address the quest… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1410.6792v1-abstract-full').style.display = 'inline'; document.getElementById('1410.6792v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1410.6792v1-abstract-full" style="display: none;"> The severe crowding towards the Galactic plane suggests that the census of nearby stars in that direction may be incomplete. Recently, Scholz reported a new M9 object at an estimated distance d~7 pc (WISE J072003.20-084651.2; hereafter WISE0720) at Galactic latitude b=2.3 degr. Our goals are to determine the physical characteristics of WISE0720, its kinematic properties, and to address the question if it is a binary object, as suggested in the discovery paper. Optical and infrared spectroscopy from the Southern African Large Telescope and Magellan, respectively, and spectral energy distribution fitting were used to determine the spectral type of WISE0720. The measured radial velocity, proper motion and parallax yielded its Galactic velocities. We also investigated if WISE0720 may show X-ray activity based on archival data. Our spectra are consistent with spectral type L0+/-1. We find no evidence for binarity, apart for a minor 2-sigma level difference in the radial velocities taken at two different epochs. The spatial velocity of WISE0720 does not connect it to any known moving group, instead it places the object with high probability in the old thin disk or in the thick disk. The spectral energy distribution fit hints at excess in the 12 and 22 micron WISE bands which may be due to a redder companion, but the same excess is visible in other late type objects, and it more likely implies a shortcoming of the models (e.g., issues with the effective wavelengths of the filters for these extremely cool objects, etc.) rather than a disk or redder companion. The optical spectrum shows some Halpha emission, indicative of stellar activity. Archival X-ray observations yield no detection. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1410.6792v1-abstract-full').style.display = 'none'; document.getElementById('1410.6792v1-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 October, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">A&A, accepted; 9 pages, 6 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1408.5424">arXiv:1408.5424</a> <span> [<a href="https://arxiv.org/pdf/1408.5424">pdf</a>, <a href="https://arxiv.org/ps/1408.5424">ps</a>, <a href="https://arxiv.org/format/1408.5424">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/10.1051/0004-6361/201424505">10.1051/0004-6361/201424505 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Temperature constraints on the coldest brown dwarf known WISE 0855-0714 </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Ivanov%2C+V+D">V. D. Ivanov</a>, <a href="/search/astro-ph?searchtype=author&query=Bayo%2C+A">A. Bayo</a>, <a href="/search/astro-ph?searchtype=author&query=Mu%C5%BEi%C4%87%2C+K">K. Mu啪i膰</a>, <a href="/search/astro-ph?searchtype=author&query=Boffin%2C+H+M+J">H. M. J. Boffin</a>, <a href="/search/astro-ph?searchtype=author&query=Allard%2C+F">F. Allard</a>, <a href="/search/astro-ph?searchtype=author&query=Homeier%2C+D">D. Homeier</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Gromadzki%2C+M">M. Gromadzki</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtev%2C+R">R. Kurtev</a>, <a href="/search/astro-ph?searchtype=author&query=Lodieu%2C+N">N. Lodieu</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+E+L">E. L. Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Mendez%2C+R+A">R. A. Mendez</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1408.5424v3-abstract-short" style="display: inline;"> Context. Nearby isolated planetary mass objects are beginning to be discovered, but their individual properties are poorly constrained because their low surface temperatures and strong molecular self-absorption make them extremely faint. Aims. We aimed to detect the near infrared emission of the coldest brown dwarf (BD) found so far, WISE0855$-$0714, located $\sim$2.2 pc away, and to improve its… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1408.5424v3-abstract-full').style.display = 'inline'; document.getElementById('1408.5424v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1408.5424v3-abstract-full" style="display: none;"> Context. Nearby isolated planetary mass objects are beginning to be discovered, but their individual properties are poorly constrained because their low surface temperatures and strong molecular self-absorption make them extremely faint. Aims. We aimed to detect the near infrared emission of the coldest brown dwarf (BD) found so far, WISE0855$-$0714, located $\sim$2.2 pc away, and to improve its temperature estimate (T$_{\rm eff}$= 225-260 K) from a comparison with state-of-the-art models of BD atmospheres. Methods. We observed the field containing WISE0855-0714 with HAWK-I at the VLT in the $Y$ band. For BDs with T$_{\rm eff}<$500\,K theoretical models predict strong signal (or rather less molecular absorption) in this band. Results. WISE0855-0714 was not detected in our Y-band images, thus placing an upper limit on its brightness to Y>24.4 mag at 3-$蟽$ level, leading to Y-[4.5]>10.5. Combining this limit with previous detections and upper limits at other wavelengths, WISE0855$-$0714 is confirmed as the reddest BD detected, further supporting its status as the coldest known brown dwarf. We applied spectral energy distribution fitting with collections of models from two independent groups for extremely cool BD atmospheres leading to an effective temperature of T$_{\rm eff}<$250\,K,. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1408.5424v3-abstract-full').style.display = 'none'; document.getElementById('1408.5424v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 October, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 August, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">4 pages, 4 figures. A&A letter Accepted</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 570, L8 (2014) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1406.3241">arXiv:1406.3241</a> <span> [<a href="https://arxiv.org/pdf/1406.3241">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> VISTA Variables in the V铆a L谩ctea (VVV): Halfway Status and Results </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hempel%2C+M">Maren Hempel</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">Dante Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%A9k%C3%A1ny%2C+I">Istv谩n D茅k谩ny</a>, <a href="/search/astro-ph?searchtype=author&query=Saito%2C+R+K">Roberto K. Saito</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+P+W">Philip W. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=Emerson%2C+J">Jim Emerson</a>, <a href="/search/astro-ph?searchtype=author&query=Ahumada%2C+A+V">Andrea V. Ahumada</a>, <a href="/search/astro-ph?searchtype=author&query=Aigrain%2C+S">Suzanne Aigrain</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso%2C+M+V">Maria Victoria Alonso</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso-Garc%C3%ADa%2C+J">Javier Alonso-Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Am%C3%B4res%2C+E+B">Eduardo B. Am么res</a>, <a href="/search/astro-ph?searchtype=author&query=Angeloni%2C+R">Rodolfo Angeloni</a>, <a href="/search/astro-ph?searchtype=author&query=Arias%2C+J">Julia Arias</a>, <a href="/search/astro-ph?searchtype=author&query=Bandyopadhyay%2C+R">Reba Bandyopadhyay</a>, <a href="/search/astro-ph?searchtype=author&query=Barb%C3%A1%2C+R+H">Rodolfo H. Barb谩</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">Beatriz Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=Baume%2C+G">Gustavo Baume</a>, <a href="/search/astro-ph?searchtype=author&query=Beamin%2C+J+C">Juan Carlos Beamin</a>, <a href="/search/astro-ph?searchtype=author&query=Bedin%2C+L">Luigi Bedin</a>, <a href="/search/astro-ph?searchtype=author&query=Bica%2C+E">Eduardo Bica</a>, <a href="/search/astro-ph?searchtype=author&query=Borissova%2C+J">Jordanka Borissova</a>, <a href="/search/astro-ph?searchtype=author&query=Bronfman%2C+L">Leonardo Bronfman</a>, <a href="/search/astro-ph?searchtype=author&query=Carraro%2C+G">Giovanni Carraro</a>, <a href="/search/astro-ph?searchtype=author&query=Catelan%2C+M">M谩rcio Catelan</a>, <a href="/search/astro-ph?searchtype=author&query=Clari%C3%A1%2C+J+J">Juan J. Clari谩</a> , et al. (67 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1406.3241v1-abstract-short" style="display: inline;"> The VISTA Variables in the V铆a L谩ctea (VVV) survey is one of six public ESO surveys, and is now in its 4th year of observing. Although far from being complete, the VVV survey has already delivered many results, some directly connected to the intended science goals (detection of variables stars, microlensing events, new star clusters), others concerning more exotic objects, e.g. novae. Now, at the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1406.3241v1-abstract-full').style.display = 'inline'; document.getElementById('1406.3241v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1406.3241v1-abstract-full" style="display: none;"> The VISTA Variables in the V铆a L谩ctea (VVV) survey is one of six public ESO surveys, and is now in its 4th year of observing. Although far from being complete, the VVV survey has already delivered many results, some directly connected to the intended science goals (detection of variables stars, microlensing events, new star clusters), others concerning more exotic objects, e.g. novae. Now, at the end of the fourth observing period, and comprising roughly 50% of the proposed observations, the actual status of the survey, as well some of the results based on the VVV data, are presented. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1406.3241v1-abstract-full').style.display = 'none'; document.getElementById('1406.3241v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 June, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5 pages, 7 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ESO Messenger 155, (2014), 29-32 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1406.0891">arXiv:1406.0891</a> <span> [<a href="https://arxiv.org/pdf/1406.0891">pdf</a>, <a href="https://arxiv.org/ps/1406.0891">ps</a>, <a href="https://arxiv.org/format/1406.0891">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"> Proper motions and brown dwarfs with the VVV survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Valentin%2C+V+D">V. D. Valentin</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtev%2C+R">R. Kurtev</a>, <a href="/search/astro-ph?searchtype=author&query=Gromadzki%2C+M">M. Gromadzki</a>, <a href="/search/astro-ph?searchtype=author&query=Ramirez%2C+K+P">K. Pe帽a Ramirez</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1406.0891v1-abstract-short" style="display: inline;"> The Vista Variables in the V铆a L谩ctea survey (VVV) is a near-IR ESO public survey devoted to study the Galactic bulge and southern inner disk covering 560 deg$^2$ on the sky. This multi-epoch and multi-wavelength survey has helped to discover the first brown dwarfs towards the Galactic center, one of the most crowded areas in the sky, and several low mass companions to known nearby stars. The mult… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1406.0891v1-abstract-full').style.display = 'inline'; document.getElementById('1406.0891v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1406.0891v1-abstract-full" style="display: none;"> The Vista Variables in the V铆a L谩ctea survey (VVV) is a near-IR ESO public survey devoted to study the Galactic bulge and southern inner disk covering 560 deg$^2$ on the sky. This multi-epoch and multi-wavelength survey has helped to discover the first brown dwarfs towards the Galactic center, one of the most crowded areas in the sky, and several low mass companions to known nearby stars. The multi-epoch information has allowed us to calculate precise parallaxes, and put some constraints on the long-term variability of these objects. We expect to discover above a hundred more brown dwarfs. The VVV survey makes a great synergy with the Gaia mission, as both will observe for a few years the same fields at different wavelengths, and as VVV is more sensitive to very red objects such as brown dwarfs, VVV might provide unique candidates to follow up eventual astrometric microlensing events thank to the exquisite astrometric precision of the Gaia mission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1406.0891v1-abstract-full').style.display = 'none'; document.getElementById('1406.0891v1-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">originally announced</span> June 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">4 pages, 2 figures. submitted to the proceedings of "Gaia and the unseen - the brown dwarf question", Torino, 24-26 March 2014, to be published in Memorie della Societa' Astronomica Italiana (SAIt), eds Ricky Smart, David Barrado, Jackie Faherty</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/1310.4072">arXiv:1310.4072</a> <span> [<a href="https://arxiv.org/pdf/1310.4072">pdf</a>, <a href="https://arxiv.org/ps/1310.4072">ps</a>, <a href="https://arxiv.org/format/1310.4072">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"> VVV High Proper Motion Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gromadzki%2C+M">M. Gromadzki</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtev%2C+R">R. Kurtev</a>, <a href="/search/astro-ph?searchtype=author&query=Folkes%2C+S">S. Folkes</a>, <a href="/search/astro-ph?searchtype=author&query=Beamin%2C+J+C">J. C. Beamin</a>, <a href="/search/astro-ph?searchtype=author&query=Ramirez%2C+K+P">K. Pena Ramirez</a>, <a href="/search/astro-ph?searchtype=author&query=Borissova%2C+J">J. Borissova</a>, <a href="/search/astro-ph?searchtype=author&query=Pinfield%2C+D">D. Pinfield</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+H">H. Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Ivanov%2C+V+D">V. D. Ivanov</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="1310.4072v1-abstract-short" style="display: inline;"> Here we present survey of proper motion stars towards the Galactic Bulge and an adjacent plane region base on VISTA-VVV data. The searching method based on cross-matching photometric Ks-band CASU catalogs. The most interesting discoveries are shown. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1310.4072v1-abstract-full" style="display: none;"> Here we present survey of proper motion stars towards the Galactic Bulge and an adjacent plane region base on VISTA-VVV data. The searching method based on cross-matching photometric Ks-band CASU catalogs. The most interesting discoveries are shown. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1310.4072v1-abstract-full').style.display = 'none'; document.getElementById('1310.4072v1-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, 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">3 pages, 1 figures. Proceedings for the conference "Brown dwarfs come of age", 2013 May 20-24, to be published in Memorie della Societa Astronomica Italiana</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1310.1996">arXiv:1310.1996</a> <span> [<a href="https://arxiv.org/pdf/1310.1996">pdf</a>, <a href="https://arxiv.org/ps/1310.1996">ps</a>, <a href="https://arxiv.org/format/1310.1996">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Stellar Variability in the VVV survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Catelan%2C+M">M. Catelan</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+P+W">P. W. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%A9k%C3%A1ny%2C+I">I. D茅k谩ny</a>, <a href="/search/astro-ph?searchtype=author&query=Saito%2C+R+K">R. K. Saito</a>, <a href="/search/astro-ph?searchtype=author&query=Angeloni%2C+R">R. Angeloni</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso-Garc%C3%ADa%2C+J">J. Alonso-Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Hempel%2C+M">M. Hempel</a>, <a href="/search/astro-ph?searchtype=author&query=Helminiak%2C+K">K. Helminiak</a>, <a href="/search/astro-ph?searchtype=author&query=Jord%C3%A1n%2C+A">A. Jord谩n</a>, <a href="/search/astro-ph?searchtype=author&query=Ramos%2C+R+C">R. Contreras Ramos</a>, <a href="/search/astro-ph?searchtype=author&query=Navarrete%2C+C">C. Navarrete</a>, <a href="/search/astro-ph?searchtype=author&query=Beam%C3%ADn%2C+J+C">J. C. Beam铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas%2C+A+F">A. F. Rojas</a>, <a href="/search/astro-ph?searchtype=author&query=Gran%2C+F">F. Gran</a>, <a href="/search/astro-ph?searchtype=author&query=Lopes%2C+C+E+F">C. E. Ferreira Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Pe%C3%B1a%2C+C+C">C. Contreras Pe帽a</a>, <a href="/search/astro-ph?searchtype=author&query=Kerins%2C+E">E. Kerins</a>, <a href="/search/astro-ph?searchtype=author&query=Huckvale%2C+L">L. Huckvale</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">M. Rejkuba</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R">R. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Mauro%2C+F">F. Mauro</a>, <a href="/search/astro-ph?searchtype=author&query=Borissova%2C+J">J. Borissova</a>, <a href="/search/astro-ph?searchtype=author&query=Amigo%2C+P">P. Amigo</a>, <a href="/search/astro-ph?searchtype=author&query=Eyheramendy%2C+S">S. Eyheramendy</a> , et al. (12 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1310.1996v2-abstract-short" style="display: inline;"> The Vista Variables in the V铆a L谩ctea (VVV) ESO Public Survey is an ongoing time-series, near-infrared (IR) survey of the Galactic bulge and an adjacent portion of the inner disk, covering 562 square degrees of the sky, using ESO's VISTA telescope. The survey has provided superb multi-color photometry in 5 broadband filters ($Z$, $Y$, $J$, $H$, and $K_s$), leading to the best map of the inner Milk… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1310.1996v2-abstract-full').style.display = 'inline'; document.getElementById('1310.1996v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1310.1996v2-abstract-full" style="display: none;"> The Vista Variables in the V铆a L谩ctea (VVV) ESO Public Survey is an ongoing time-series, near-infrared (IR) survey of the Galactic bulge and an adjacent portion of the inner disk, covering 562 square degrees of the sky, using ESO's VISTA telescope. The survey has provided superb multi-color photometry in 5 broadband filters ($Z$, $Y$, $J$, $H$, and $K_s$), leading to the best map of the inner Milky Way ever obtained, particularly in the near-IR. The main variability part of the survey, which is focused on $K_s$-band observations, is currently underway, with bulge fields having been observed between 31 and 70 times, and disk fields between 17 and 36 times. When the survey is complete, bulge (disk) fields will have been observed up to a total of 100 (60) times, providing unprecedented depth and time coverage. Here we provide a first overview of stellar variability in the VVV data, including examples of the light curves that have been collected thus far, scientific applications, and our efforts towards the automated classification of VVV light curves. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1310.1996v2-abstract-full').style.display = 'none'; document.getElementById('1310.1996v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 November, 2013; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 October, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Presented at the "40 Years of Variable Stars: A Celebration of Contributions by Horace A. Smith" conference (arXiv:1310.0149). 49 pages, 28 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> HASMITH/2013/17 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1309.4301">arXiv:1309.4301</a> <span> [<a href="https://arxiv.org/pdf/1309.4301">pdf</a>, <a href="https://arxiv.org/format/1309.4301">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/10.1051/0004-6361/201321045">10.1051/0004-6361/201321045 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery of New Companions to High Proper Motion Stars from the VVV Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ivanov%2C+V+D">Valentin D. Ivanov</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">Dante Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Hempel%2C+M">Maren Hempel</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtev%2C+R">Radostin Kurtev</a>, <a href="/search/astro-ph?searchtype=author&query=Toledo%2C+I">Ignacio Toledo</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=Alonso-Garcia%2C+J">Javier Alonso-Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Beamin%2C+J+C">Juan Carlos Beamin</a>, <a href="/search/astro-ph?searchtype=author&query=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=Chene%2C+A">Andre-Nicolas Chene</a>, <a href="/search/astro-ph?searchtype=author&query=Emerson%2C+J">Jim Emerson</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=Lucas%2C+P+W">Phillip W. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+E+L">Eduardo L. Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">Marina Rejkuba</a>, <a href="/search/astro-ph?searchtype=author&query=Gromadzki%2C+M">Mariusz Gromadzki</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1309.4301v1-abstract-short" style="display: inline;"> [abridged] The severe crowding in the direction of the inner Milky Way suggests that the census of stars within a few tens of parsecs in that direction may not be complete. We search for new nearby objects companions of known high proper motion (HPM) stars located towards the densest regions of the Southern Milky Way where the background contamination presented a major problem to previous works.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1309.4301v1-abstract-full').style.display = 'inline'; document.getElementById('1309.4301v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1309.4301v1-abstract-full" style="display: none;"> [abridged] The severe crowding in the direction of the inner Milky Way suggests that the census of stars within a few tens of parsecs in that direction may not be complete. We search for new nearby objects companions of known high proper motion (HPM) stars located towards the densest regions of the Southern Milky Way where the background contamination presented a major problem to previous works. The common proper motion (PM) method was used--we inspected the area around 167 known HPM (>=200 mas/yr) stars: 67 in the disk and 100 in the bulge. Multi-epoch images were provided by 2MASS and the VISTA Variables in Via Lactea (VVV). The VVV is a new on-going ZYJHKs plus multi-epoch Ks survey of ~562 deg^2 of Milky Way's bulge and inner Southern disk. Seven new co-moving companions were discovered around known HPM stars; six known co-moving pairs were recovered; a pair of stars that was thought to be co-moving was found to have different proper motions; published HPMs of eight stars were not confirmed; last but not least, spectral types ranging from G8V to M5V were derived from new infrared spectroscopy for seventeen stars, members of the co-moving pairs. The seven newly discovered stars constitute ~4% of the nearby HPM star list but this is not a firm limit on the HPM star incompleteness because our starting point--the HPM list assembled from the literature--is incomplete itself, missing many nearby HPM M and L type objects, and it is contaminated with non-HPM stars. We have demonstrated, that the superior sub-arcsec spatial resolution, with respect to previous surveys, allows the VVV to examine further the binary nature nature of known HPM stars. The >=5 yr span of VVV will provide sufficient baseline for finding new HPM stars from VVV data alone. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1309.4301v1-abstract-full').style.display = 'none'; document.getElementById('1309.4301v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 September, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A; 14 pages, 3 figures, 6 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1308.3216">arXiv:1308.3216</a> <span> [<a href="https://arxiv.org/pdf/1308.3216">pdf</a>, <a href="https://arxiv.org/ps/1308.3216">ps</a>, <a href="https://arxiv.org/format/1308.3216">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/10.1051/0004-6361/201322190">10.1051/0004-6361/201322190 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> One more neighbor: The first brown dwarf in the VVV survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Gromadzki%2C+M">M. Gromadzki</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtev%2C+R">R. Kurtev</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=Beletsky%2C+Y">Y. Beletsky</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+P">P. Lucas</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=Borissova%2C+J">J. Borissova</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1308.3216v1-abstract-short" style="display: inline;"> Context. The discovery of brown dwarfs (BDs) in the solar neighborhood and young star clusters has helped to constraint the low-mass end of the stellar mass function and the initial mass function. We use data of the Vista Variables in the V铆a L谩ctea (VVV), a near-infrared (NIR) multiwavelength (Z Y J H Ks) multi-epoch (Ks) ESO Public Survey mapping the Milky Way bulge and southern Galactic plane t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1308.3216v1-abstract-full').style.display = 'inline'; document.getElementById('1308.3216v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1308.3216v1-abstract-full" style="display: none;"> Context. The discovery of brown dwarfs (BDs) in the solar neighborhood and young star clusters has helped to constraint the low-mass end of the stellar mass function and the initial mass function. We use data of the Vista Variables in the V铆a L谩ctea (VVV), a near-infrared (NIR) multiwavelength (Z Y J H Ks) multi-epoch (Ks) ESO Public Survey mapping the Milky Way bulge and southern Galactic plane to search for nearby BDs. Aims. The ultimate aim of the project is to improve the completeness of the census of nearby stellar and substellar objects towards the Galactic bulge and inner disk regions. Methods. Taking advantage of the homogeneous sample of VVV multi-epoch data, we identified stars with high proper motion (> 0.1"/yr), and then selected low-mass objects using NIR colors. We searched for a possible parallax signature using the all available Ks band epochs. We set some constraints on the month-to-year scale Ks band variability of our candidates, and even searched for possible transiting companions. We obtained NIR spectra to properly classify spectral type and then the physical properties of the final list of candidates. Results. We report the discovery of VVV BD001, a new member of the local volume-limited sample (within 20pc from the sun) with well defined proper motion, distance, and luminosity. The spectral type of this new object is an L5+-1, unusually blue dwarf. The proper motion for this BD is PM(伪)=-0.5455+-0.004 "/yr, PM(未)=-0.3255+-0.004 "/yr, and it has a parallax of 57+-4 mas which translates into a distance of 17.5 +- 1.1 pc. VVV BD001 shows no evidence of variability (螖Ks <0.05mag) over two years, especially constrained on a six month scale during the year 2012. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1308.3216v1-abstract-full').style.display = 'none'; document.getElementById('1308.3216v1-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> 14 August, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5 pages, 4 figures, 1 table, Accepted for publication in Astronomy and Astrophysics Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1305.5902">arXiv:1305.5902</a> <span> [<a href="https://arxiv.org/pdf/1305.5902">pdf</a>, <a href="https://arxiv.org/format/1305.5902">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/10.1051/0004-6361/201220046">10.1051/0004-6361/201220046 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Milky Way Demographics with the VVV Survey II. Color Transformations and Near-Infrared Photometry for 136 Million Stars in the Southern Galactic Disk </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Soto%2C+M">M. Soto</a>, <a href="/search/astro-ph?searchtype=author&query=Barba%2C+R">R. Barba</a>, <a href="/search/astro-ph?searchtype=author&query=Gunthardt%2C+G">G. Gunthardt</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+P">P. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=Majaess%2C+D">D. Majaess</a>, <a href="/search/astro-ph?searchtype=author&query=Irwin%2C+M">M. Irwin</a>, <a href="/search/astro-ph?searchtype=author&query=Emerson%2C+J+P">J. P. Emerson</a>, <a href="/search/astro-ph?searchtype=author&query=Gonzalez-Solares%2C+E">E. Gonzalez-Solares</a>, <a href="/search/astro-ph?searchtype=author&query=Hempel%2C+M">M. Hempel</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=Gurovich%2C+S">S. Gurovich</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Lopes%2C+A">A. Roman-Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Moni-Bidin%2C+C">C. Moni-Bidin</a>, <a href="/search/astro-ph?searchtype=author&query=Santucho%2C+M+V">M. V. Santucho</a>, <a href="/search/astro-ph?searchtype=author&query=Borissova%2C+J">J. Borissova</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtev%2C+R">R. Kurtev</a>, <a href="/search/astro-ph?searchtype=author&query=Toledo%2C+I">I. Toledo</a>, <a href="/search/astro-ph?searchtype=author&query=Geisler%2C+D">D. Geisler</a>, <a href="/search/astro-ph?searchtype=author&query=Dominguez%2C+M">M. Dominguez</a>, <a href="/search/astro-ph?searchtype=author&query=Beamin%2C+J+C">J. C. 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="1305.5902v1-abstract-short" style="display: inline;"> The new multi-epoch near-infrared VVV survey (VISTA Variables in the Via Lactea) is sampling 562 sq. deg of the Galactic bulge and adjacent regions of the disk. Accurate astrometry established for the region surveyed allows the VVV data to be merged with overlapping surveys (e.g., GLIMPSE, WISE, 2MASS, etc.), thereby enabling the construction of longer baseline spectral energy distributions for as… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1305.5902v1-abstract-full').style.display = 'inline'; document.getElementById('1305.5902v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1305.5902v1-abstract-full" style="display: none;"> The new multi-epoch near-infrared VVV survey (VISTA Variables in the Via Lactea) is sampling 562 sq. deg of the Galactic bulge and adjacent regions of the disk. Accurate astrometry established for the region surveyed allows the VVV data to be merged with overlapping surveys (e.g., GLIMPSE, WISE, 2MASS, etc.), thereby enabling the construction of longer baseline spectral energy distributions for astronomical targets. However, in order to maximize use of the VVV data, a set of transformation equations are required to place the VVV JHKs photometry onto the 2MASS system. The impetus for this work is to develop those transformations via a comparison of 2MASS targets in 152 VVV fields sampling the Galactic disk. The transformation coefficients derived exhibit a reliance on variables such as extinction. The transformed data were subsequently employed to establish a mean reddening law of E_{J-H}/E_{H-Ks}=2.13 +/- 0.04, which is the most precise determination to date and merely emphasizes the pertinence of the VVV data for determining such important parameters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1305.5902v1-abstract-full').style.display = 'none'; document.getElementById('1305.5902v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 May, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">24 pages, 12 figures, published 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 552, A101 (2013) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1304.2673">arXiv:1304.2673</a> <span> [<a href="https://arxiv.org/pdf/1304.2673">pdf</a>, <a href="https://arxiv.org/ps/1304.2673">ps</a>, <a href="https://arxiv.org/format/1304.2673">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201321260">10.1051/0004-6361/201321260 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A near-infrared catalogue of the Galactic novae in the VVV survey area </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Saito%2C+R+K">R. K. Saito</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Angeloni%2C+R">R. Angeloni</a>, <a href="/search/astro-ph?searchtype=author&query=Catelan%2C+M">M. Catelan</a>, <a href="/search/astro-ph?searchtype=author&query=Beamin%2C+J+C">J. C. Beamin</a>, <a href="/search/astro-ph?searchtype=author&query=Borissova%2C+J">J. Borissova</a>, <a href="/search/astro-ph?searchtype=author&query=Dekany%2C+I">I. Dekany</a>, <a href="/search/astro-ph?searchtype=author&query=Kerins%2C+E">E. Kerins</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtev%2C+R">R. Kurtev</a>, <a href="/search/astro-ph?searchtype=author&query=Mennickent%2C+R+E">R. E. Mennickent</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1304.2673v1-abstract-short" style="display: inline;"> Near-IR data of Classical Novae contain useful information about the ejected gas mass and the thermal emission by dust formed during eruption, and provide independent methods to classify the objects according to the colour of their progenitors, and the fading rate and features seen after eruption. The VISTA Variables in the Via Lactea survey (VVV) is a near-IR ESO Public Survey mapping the MW bulg… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1304.2673v1-abstract-full').style.display = 'inline'; document.getElementById('1304.2673v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1304.2673v1-abstract-full" style="display: none;"> Near-IR data of Classical Novae contain useful information about the ejected gas mass and the thermal emission by dust formed during eruption, and provide independent methods to classify the objects according to the colour of their progenitors, and the fading rate and features seen after eruption. The VISTA Variables in the Via Lactea survey (VVV) is a near-IR ESO Public Survey mapping the MW bulge and southern plane. Data taken during 2010-2011 covered the entire area in the JHKs bands plus some epochs in Ks-band of the ongoing VVV variability campaign. We used the novae list provided by VSX/AAVSO catalogue to search for all objects within the VVV area. We used the VVV data to create a near-IR catalogue of the known Galactic novae in the 562 sq.deg. area covered by VVV. The VVV near-IR catalogue of novae contains JHKs photometry of 93 objects completed as of December 2012. We also checked in the ongoing VVV variability campaign for the light-curves of novae that erupted in the last years. VVV images can also be used to discover and study novae by searching for the expanding shell. Since objects are seen at different distances and reddening levels, the colour-magnitude and colour-colour diagrams show the novae spread in magnitude as well as in colour. Dereddened colours and reddening-free indices were used with caution and cannot be a good approach in all cases since the distance and spectral features prevent more conclusive results for some extreme objects. Light-curves for some recent novae are presented. Thanks to its high spatial resolution in the near-IR, and large Ks-range, the VVV survey can be a major contributor for the search and study of novae in the most crowded and high-extinction regions of the Milky Way. The VVV survey area contains ~35 of all known novae in the Galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1304.2673v1-abstract-full').style.display = 'none'; document.getElementById('1304.2673v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 April, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astronomy and Astrophysics (Section 14: Catalogs and data)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1111.5511">arXiv:1111.5511</a> <span> [<a href="https://arxiv.org/pdf/1111.5511">pdf</a>, <a href="https://arxiv.org/ps/1111.5511">ps</a>, <a href="https://arxiv.org/format/1111.5511">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201118407">10.1051/0004-6361/201118407 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> VVV DR1: The First Data Release of the Milky Way Bulge and Southern Plane from the Near-Infrared ESO Public Survey VISTA Variables in the Via Lactea </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Saito%2C+R+K">R. K. Saito</a>, <a href="/search/astro-ph?searchtype=author&query=Hempel%2C+M">M. Hempel</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+P+W">P. W. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">M. Rejkuba</a>, <a href="/search/astro-ph?searchtype=author&query=Toledo%2C+I">I. Toledo</a>, <a href="/search/astro-ph?searchtype=author&query=Gonzalez%2C+O+A">O. A. Gonzalez</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso-Garcia%2C+J">J. Alonso-Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Irwin%2C+M+J">M. J. Irwin</a>, <a href="/search/astro-ph?searchtype=author&query=Gonzalez-Solares%2C+E">E. Gonzalez-Solares</a>, <a href="/search/astro-ph?searchtype=author&query=Hodgkin%2C+S+T">S. T. Hodgkin</a>, <a href="/search/astro-ph?searchtype=author&query=Lewis%2C+J+R">J. R. Lewis</a>, <a href="/search/astro-ph?searchtype=author&query=Cross%2C+N">N. Cross</a>, <a href="/search/astro-ph?searchtype=author&query=Ivanov%2C+V+D">V. D. Ivanov</a>, <a href="/search/astro-ph?searchtype=author&query=Kerins%2C+E">E. Kerins</a>, <a href="/search/astro-ph?searchtype=author&query=Emerson%2C+J+P">J. P. Emerson</a>, <a href="/search/astro-ph?searchtype=author&query=Soto%2C+M">M. Soto</a>, <a href="/search/astro-ph?searchtype=author&query=Amores%2C+E+B">E. B. Amores</a>, <a href="/search/astro-ph?searchtype=author&query=Gurovich%2C+S">S. Gurovich</a>, <a href="/search/astro-ph?searchtype=author&query=Dekany%2C+I">I. Dekany</a>, <a href="/search/astro-ph?searchtype=author&query=Angeloni%2C+R">R. Angeloni</a>, <a href="/search/astro-ph?searchtype=author&query=Beamin%2C+J+C">J. C. Beamin</a>, <a href="/search/astro-ph?searchtype=author&query=Catelan%2C+M">M. Catelan</a>, <a href="/search/astro-ph?searchtype=author&query=Padilla%2C+N">N. Padilla</a>, <a href="/search/astro-ph?searchtype=author&query=Zoccali%2C+M">M. Zoccali</a> , et al. (85 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1111.5511v1-abstract-short" style="display: inline;"> The ESO Public Survey VISTA Variables in the Via Lactea (VVV) started in 2010. VVV targets 562 sq. deg in the Galactic bulge and an adjacent plane region and is expected to run for ~5 years. In this paper we describe the progress of the survey observations in the first observing season, the observing strategy and quality of the data obtained. The observations are carried out on the 4-m VISTA teles… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1111.5511v1-abstract-full').style.display = 'inline'; document.getElementById('1111.5511v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1111.5511v1-abstract-full" style="display: none;"> The ESO Public Survey VISTA Variables in the Via Lactea (VVV) started in 2010. VVV targets 562 sq. deg in the Galactic bulge and an adjacent plane region and is expected to run for ~5 years. In this paper we describe the progress of the survey observations in the first observing season, the observing strategy and quality of the data obtained. The observations are carried out on the 4-m VISTA telescope in the ZYJHKs filters. In addition to the multi-band imaging the variability monitoring campaign in the Ks filter has started. Data reduction is carried out using the pipeline at the Cambridge Astronomical Survey Unit. The photometric and astrometric calibration is performed via the numerous 2MASS sources observed in each pointing. The first data release contains the aperture photometry and astrometric catalogues for 348 individual pointings in the ZYJHKs filters taken in the 2010 observing season. The typical image quality is ~0.9-1.0". The stringent photometric and image quality requirements of the survey are satisfied in 100% of the JHKs images in the disk area and 90% of the JHKs images in the bulge area. The completeness in the Z and Y images is 84% in the disk, and 40% in the bulge. The first season catalogues contain 1.28x10^8 stellar sources in the bulge and 1.68x10^8 in the disk area detected in at least one of the photometric bands. The combined, multi-band catalogues contain more than 1.63x10^8 stellar sources. About 10% of these are double detections due to overlapping adjacent pointings. These overlapping multiple detections are used to characterise the quality of the data. The images in the JHKs bands extend typically ~4 mag deeper than 2MASS. The magnitude limit and photometric quality depend strongly on crowding in the inner Galactic regions. The astrometry for Ks=15-18 mag has rms ~35-175 mas. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1111.5511v1-abstract-full').style.display = 'none'; document.getElementById('1111.5511v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 November, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2011. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astronomy and Astrophysics (Section 14: Catalogs and data)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1105.1119">arXiv:1105.1119</a> <span> [<a href="https://arxiv.org/pdf/1105.1119">pdf</a>, <a href="https://arxiv.org/format/1105.1119">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> The Vista Variables in the Via Lactea (VVV) ESO Public Survey: Current Status and First Results </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Catelan%2C+M">M. Catelan</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+P+W">P. W. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso-Garcia%2C+J">J. Alonso-Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Angeloni%2C+R">R. Angeloni</a>, <a href="/search/astro-ph?searchtype=author&query=Beamin%2C+J+C">J. C. Beamin</a>, <a href="/search/astro-ph?searchtype=author&query=Bonatto%2C+C">C. Bonatto</a>, <a href="/search/astro-ph?searchtype=author&query=Borissova%2C+J">J. Borissova</a>, <a href="/search/astro-ph?searchtype=author&query=Contreras%2C+C">C. Contreras</a>, <a href="/search/astro-ph?searchtype=author&query=Cross%2C+N">N. Cross</a>, <a href="/search/astro-ph?searchtype=author&query=Dekany%2C+I">I. Dekany</a>, <a href="/search/astro-ph?searchtype=author&query=Emerson%2C+J+P">J. P. Emerson</a>, <a href="/search/astro-ph?searchtype=author&query=Eyheramendy%2C+S">S. Eyheramendy</a>, <a href="/search/astro-ph?searchtype=author&query=Geisler%2C+D">D. Geisler</a>, <a href="/search/astro-ph?searchtype=author&query=Gonzalez-Solares%2C+E">E. Gonzalez-Solares</a>, <a href="/search/astro-ph?searchtype=author&query=Helminiak%2C+K+G">K. G. Helminiak</a>, <a href="/search/astro-ph?searchtype=author&query=Hempel%2C+M">M. Hempel</a>, <a href="/search/astro-ph?searchtype=author&query=Irwin%2C+M+J">M. J. Irwin</a>, <a href="/search/astro-ph?searchtype=author&query=Ivanov%2C+V+D">V. D. Ivanov</a>, <a href="/search/astro-ph?searchtype=author&query=Jordan%2C+A">A. Jordan</a>, <a href="/search/astro-ph?searchtype=author&query=Kerins%2C+E">E. Kerins</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtev%2C+R">R. Kurtev</a>, <a href="/search/astro-ph?searchtype=author&query=Mauro%2C+F">F. Mauro</a>, <a href="/search/astro-ph?searchtype=author&query=Bidin%2C+C+M">C. Moni Bidin</a>, <a href="/search/astro-ph?searchtype=author&query=Navarrete%2C+C">C. Navarrete</a> , et al. (7 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1105.1119v2-abstract-short" style="display: inline;"> Vista Variables in the Via Lactea (VVV) is an ESO Public Survey that is performing a variability survey of the Galactic bulge and part of the inner disk using ESO's Visible and Infrared Survey Telescope for Astronomy (VISTA). The survey covers 520 deg^2 of sky area in the ZYJHK_S filters, for a total observing time of 1929 hours, including ~ 10^9 point sources and an estimated ~ 10^6 variable star… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1105.1119v2-abstract-full').style.display = 'inline'; document.getElementById('1105.1119v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1105.1119v2-abstract-full" style="display: none;"> Vista Variables in the Via Lactea (VVV) is an ESO Public Survey that is performing a variability survey of the Galactic bulge and part of the inner disk using ESO's Visible and Infrared Survey Telescope for Astronomy (VISTA). The survey covers 520 deg^2 of sky area in the ZYJHK_S filters, for a total observing time of 1929 hours, including ~ 10^9 point sources and an estimated ~ 10^6 variable stars. Here we describe the current status of the VVV Survey, in addition to a variety of new results based on VVV data, including light curves for variable stars, newly discovered globular clusters, open clusters, and associations. A set of reddening-free indices based on the ZYJHK_S system is also introduced. Finally, we provide an overview of the VVV Templates Project, whose main goal is to derive well-defined light curve templates in the near-IR, for the automated classification of VVV light curves. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1105.1119v2-abstract-full').style.display = 'none'; document.getElementById('1105.1119v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 June, 2011; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 May, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2011. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 18 figures. To appear in the Carnegie Observatories Astrophysics Series, Volume 5</span> </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg> <a href="https://info.arxiv.org/help/contact.html"> Contact</a> </li> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>subscribe to arXiv mailings</title><desc>Click here to subscribe</desc><path d="M476 3.2L12.5 270.6c-18.1 10.4-15.8 35.6 2.2 43.2L121 358.4l287.3-253.2c5.5-4.9 13.3 2.6 8.6 8.3L176 407v80.5c0 23.6 28.5 32.9 42.5 15.8L282 426l124.6 52.2c14.2 6 30.4-2.9 33-18.2l72-432C515 7.8 493.3-6.8 476 3.2z"/></svg> <a href="https://info.arxiv.org/help/subscribe"> Subscribe</a> </li> </ul> </div> </div> </div>   <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/license/index.html">Copyright</a></li> <li><a href="https://info.arxiv.org/help/policies/privacy_policy.html">Privacy Policy</a></li> </ul> </div> <div class="column sorry-app-links"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/web_accessibility.html">Web Accessibility Assistance</a></li> <li> <p class="help"> <a class="a11y-main-link" href="https://status.arxiv.org" target="_blank">arXiv Operational Status <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 256 512" class="icon filter-dark_grey" role="presentation"><path d="M224.3 273l-136 136c-9.4 9.4-24.6 9.4-33.9 0l-22.6-22.6c-9.4-9.4-9.4-24.6 0-33.9l96.4-96.4-96.4-96.4c-9.4-9.4-9.4-24.6 0-33.9L54.3 103c9.4-9.4 24.6-9.4 33.9 0l136 136c9.5 9.4 9.5 24.6.1 34z"/></svg></a><br> Get status notifications via <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/email/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg>email</a> or <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/slack/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 448 512" class="icon filter-black" role="presentation"><path d="M94.12 315.1c0 25.9-21.16 47.06-47.06 47.06S0 341 0 315.1c0-25.9 21.16-47.06 47.06-47.06h47.06v47.06zm23.72 0c0-25.9 21.16-47.06 47.06-47.06s47.06 21.16 47.06 47.06v117.84c0 25.9-21.16 47.06-47.06 47.06s-47.06-21.16-47.06-47.06V315.1zm47.06-188.98c-25.9 0-47.06-21.16-47.06-47.06S139 32 164.9 32s47.06 21.16 47.06 47.06v47.06H164.9zm0 23.72c25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06H47.06C21.16 243.96 0 222.8 0 196.9s21.16-47.06 47.06-47.06H164.9zm188.98 47.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06h-47.06V196.9zm-23.72 0c0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06V79.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06V196.9zM283.1 385.88c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06v-47.06h47.06zm0-23.72c-25.9 0-47.06-21.16-47.06-47.06 0-25.9 21.16-47.06 47.06-47.06h117.84c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06H283.1z"/></svg>slack</a> </p> </li> </ul> </div> </div> </div>  </div> </footer> <script src="https://static.arxiv.org/static/base/1.0.0a5/js/member_acknowledgement.js"></script> </body> </html>

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