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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/2410.19985">arXiv:2410.19985</a> <span> [<a href="https://arxiv.org/pdf/2410.19985">pdf</a>, <a href="https://arxiv.org/format/2410.19985">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The Galaxy Zoo Catalogs for the Galaxy And Mass Assembly (GAMA) Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B+W">Benne W. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Robertson%2C+C">Clayton Robertson</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K">Kyle Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Pimbblet%2C+K+A">Kevin A. Pimbblet</a>, <a href="/search/astro-ph?searchtype=author&query=Casura%2C+S">Sarah Casura</a>, <a href="/search/astro-ph?searchtype=author&query=Sansom%2C+A+E">Anne E. Sansom</a>, <a href="/search/astro-ph?searchtype=author&query=Patel%2C+D">Divya Patel</a>, <a href="/search/astro-ph?searchtype=author&query=Butrum%2C+T">Trevor Butrum</a>, <a href="/search/astro-ph?searchtype=author&query=Glass%2C+D+H+W">David H. W. Glass</a>, <a href="/search/astro-ph?searchtype=author&query=Kelvin%2C+L">Lee Kelvin</a>, <a href="/search/astro-ph?searchtype=author&query=Baldry%2C+I+K">Ivan K. Baldry</a>, <a href="/search/astro-ph?searchtype=author&query=De+Propris%2C+R">Roberto De Propris</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S">Steven Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Masters%2C+K">Karen Masters</a>, <a href="/search/astro-ph?searchtype=author&query=Stone%2C+M">Maria Stone</a>, <a href="/search/astro-ph?searchtype=author&query=Hardin%2C+T">Tim Hardin</a>, <a href="/search/astro-ph?searchtype=author&query=Walmsley%2C+M">Mike Walmsley</a>, <a href="/search/astro-ph?searchtype=author&query=Liske%2C+J">Jochen Liske</a>, <a href="/search/astro-ph?searchtype=author&query=Adnan%2C+S+M+R">S M Rafee Adnan</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="2410.19985v1-abstract-short" style="display: inline;"> Galaxy Zoo is an online project to classify morphological features in extra-galactic imaging surveys with public voting. In this paper, we compare the classifications made for two different surveys, the Dark Energy Spectroscopic Instrument (DESI) imaging survey and a part of the Kilo-Degree Survey (KiDS), in the equatorial fields of the Galaxy And Mass Assembly (GAMA) survey. Our aim is to cross-v… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.19985v1-abstract-full').style.display = 'inline'; document.getElementById('2410.19985v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.19985v1-abstract-full" style="display: none;"> Galaxy Zoo is an online project to classify morphological features in extra-galactic imaging surveys with public voting. In this paper, we compare the classifications made for two different surveys, the Dark Energy Spectroscopic Instrument (DESI) imaging survey and a part of the Kilo-Degree Survey (KiDS), in the equatorial fields of the Galaxy And Mass Assembly (GAMA) survey. Our aim is to cross-validate and compare the classifications based on different imaging quality and depth. We find that generally the voting agrees globally but with substantial scatter i.e. substantial differences for individual galaxies. There is a notable higher voting fraction in favor of ``smooth'' galaxies in the DESI+\rev{\sc zoobot} classifications, most likely due to the difference between imaging depth. DESI imaging is shallower and slightly lower resolution than KiDS and the Galaxy Zoo images do not reveal details such as disk features \rev{and thus are missed in the {\sc zoobot} training sample}. \rev{We check against expert visual classifications and find good agreement with KiDS-based Galaxy Zoo voting.} We reproduce the results from Porter-Temple+ (2022), on the dependence of stellar mass, star-formation, and specific star-formation on the number of spiral arms. This shows that once corrected for redshift, the DESI Galaxy Zoo and KiDS Galaxy Zoo classifications agree well on population properties. The zoobot cross-validation increases confidence in its ability to compliment Galaxy Zoo classifications and its ability for transfer learning across surveys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.19985v1-abstract-full').style.display = 'none'; document.getElementById('2410.19985v1-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 22 figures, 8 tables, accepted for publication in PASA</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.15619">arXiv:2403.15619</a> <span> [<a href="https://arxiv.org/pdf/2403.15619">pdf</a>, <a href="https://arxiv.org/format/2403.15619">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Ground- and Space-Based Dust Observations of VV 191 Overlapping Galaxy Pair </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Robertson%2C+C">C. Robertson</a>, <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B">B. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Young%2C+J">J. Young</a>, <a href="/search/astro-ph?searchtype=author&query=Keel%2C+W">W. Keel</a>, <a href="/search/astro-ph?searchtype=author&query=Berkheimer%2C+J">J. Berkheimer</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K">K. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C">C. Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=Frye%2C+B">B. Frye</a>, <a href="/search/astro-ph?searchtype=author&query=Grogin%2C+N">N. Grogin</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A">A. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Nasr%2C+C">C. Nasr</a>, <a href="/search/astro-ph?searchtype=author&query=Patel%2C+D">D. Patel</a>, <a href="/search/astro-ph?searchtype=author&query=Roemer%2C+W">W. Roemer</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+D">D. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Windhorst%2C+R">R. Windhorst</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="2403.15619v1-abstract-short" style="display: inline;"> The Balmer decrement (H$伪$/H$尾$) provides a constraint on attenuation, the cumulative effects of dust grains in the ISM. The ratio is a reliable spectroscopic tool for deriving the dust properties of galaxies that determine many different quantities such as star formation rate, metallicity, and SED models. Here we measure independently both the attenuation and H$伪$/H$尾$ of an occulting galaxy pair… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.15619v1-abstract-full').style.display = 'inline'; document.getElementById('2403.15619v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.15619v1-abstract-full" style="display: none;"> The Balmer decrement (H$伪$/H$尾$) provides a constraint on attenuation, the cumulative effects of dust grains in the ISM. The ratio is a reliable spectroscopic tool for deriving the dust properties of galaxies that determine many different quantities such as star formation rate, metallicity, and SED models. Here we measure independently both the attenuation and H$伪$/H$尾$ of an occulting galaxy pair: VV 191. Attenuation measurements in the visible spectrum (A$_{V,stars}$) from dust maps derived from the F606W filter of HST and the F090W filter of JWST are matched with spaxel-by-spaxel H$伪$/H$尾$ observations from the George and Cynthia Mitchell Spectrograph (GCMS) of the McDonald Observatory. The 0.5 to 0.7 micron bandpass covers the Balmer lines for VV 191. The dust maps of JWST and HST provide the high sensitivity necessary for comparisons and tracking trends of the geometrically favorable galaxy. We present maps and plots of the Balmer lines for the VV 191 galaxy pair and for a specific region highlighting dust lanes for VV 191b in the overlap region. We compute A$_{V, HII}$ from H$伪$/H$尾$ and plot both quantities against A$_{V, stars}$. Our results show that regions with higher dust content, residing closer to the spiral center, dominate ionized gas attenuation, leading to an overestimation of A$_{V, HII}$ by a factor or 2. Further out in the spiral arms, the lower dust content leads to more agreement between the attenuations, indicating lower SFR and larger contribution from older stars to the stellar continuum outside the Petrosian radius. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.15619v1-abstract-full').style.display = 'none'; document.getElementById('2403.15619v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">21 pages, 14 figures, 2 tables, accepted for publication by 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/2309.16875">arXiv:2309.16875</a> <span> [<a href="https://arxiv.org/pdf/2309.16875">pdf</a>, <a href="https://arxiv.org/format/2309.16875">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Galaxy And Mass Assembly: The xSAGA Galaxy Complement in Nearby Galaxy Groups </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B+W">B. W. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Phillipps%2C+S">S. Phillipps</a>, <a href="/search/astro-ph?searchtype=author&query=Weerasooriya%2C+S">S. Weerasooriya</a>, <a href="/search/astro-ph?searchtype=author&query=Bovill%2C+M+S">M. S. Bovill</a>, <a href="/search/astro-ph?searchtype=author&query=Brough%2C+S">S. Brough</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+M+J+I">M. J. I. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Robertson%2C+C">C. Robertson</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K">K. Cook</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="2309.16875v2-abstract-short" style="display: inline;"> Groups of galaxies are the intermediate density environment in which much of the evolution of galaxies is thought to take place. In spectroscopic redshift surveys, one can identify these as close spatial redshift associations. However, spectroscopic surveys will always be more limited in luminosity and completeness than imaging ones. Here we combine the Galaxy And Mass Assembly group catalogue wit… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.16875v2-abstract-full').style.display = 'inline'; document.getElementById('2309.16875v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.16875v2-abstract-full" style="display: none;"> Groups of galaxies are the intermediate density environment in which much of the evolution of galaxies is thought to take place. In spectroscopic redshift surveys, one can identify these as close spatial redshift associations. However, spectroscopic surveys will always be more limited in luminosity and completeness than imaging ones. Here we combine the Galaxy And Mass Assembly group catalogue with the extended Satellites Around Galactic Analogues (xSAGA) catalogue of Machine Learning identified low-redshift satellite galaxies. We find 1825 xSAGA galaxies within the bounds of the GAMA equatorial fields (m < 21), 1562 of which could have a counterpart in the GAMA spectroscopic catalogue (m < 19.8). Of these, 1326 do have a GAMA counterpart with 974 below z=0.03 (true positives) and 352 above (false positives). By crosscorrelating the GAMA group catalogue with the xSAGA catalogue, we can extend and characterize the satellite content of GAMA galaxy groups. We find that most groups have <5 xSAGA galaxies associated with them but richer groups may have more. Each additional xSAGA galaxy contributes only a small fraction of the group's total stellar mass (<<10%). Selecting GAMA groups that resemble the Milky Way halo, with a few (<4) bright galaxies, we find xSAGA can add a magnitude fainter sources to a group and that the Local Group does not stand out in the number of bright satellites. We explore the quiescent fraction of xSAGA galaxies in GAMA groups and find a good agreement with the literature. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.16875v2-abstract-full').style.display = 'none'; document.getElementById('2309.16875v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">11 pages, 13 Figures, 2 Tables, accepted by MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.05835">arXiv:2309.05835</a> <span> [<a href="https://arxiv.org/pdf/2309.05835">pdf</a>, <a href="https://arxiv.org/format/2309.05835">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Cosmic Evolution Early Release Science Survey (CEERS): Multi-classing Galactic Dwarf Stars in the deep JWST/NIRCam </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B+W">B. W. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Hsu%2C+C">Chih-Chun Hsu</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N">Nimish Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Bisigello%2C+L">Laura Bisigello</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Vega%2C+A">Alexander de la Vega</a>, <a href="/search/astro-ph?searchtype=author&query=Haro%2C+P+A">Pablo Arrabal Haro</a>, <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M">Micaela Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">Mark Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">Steven L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Kartaltepe%2C+J+S">Jeyhan S. Kartaltepe</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Papovich%2C+C">Casey Papovich</a>, <a href="/search/astro-ph?searchtype=author&query=Pirzkal%2C+N">Nor Pirzkal</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K">Kyle Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Robertson%2C+C">Clayton Robertson</a>, <a href="/search/astro-ph?searchtype=author&query=Casey%2C+C+M">Caitlin M Casey</a>, <a href="/search/astro-ph?searchtype=author&query=Aganze%2C+C">Christian Aganze</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A9rez-Gonz%C3%A1lez%2C+P+G">Pablo G. P茅rez-Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+R+A">Ray A. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=Jogee%2C+S">Shardha Jogee</a>, <a href="/search/astro-ph?searchtype=author&query=Wilkins%2C+S">Stephen Wilkins</a>, <a href="/search/astro-ph?searchtype=author&query=Burgarella%2C+D">Denis Burgarella</a>, <a href="/search/astro-ph?searchtype=author&query=Kirkpatrick%2C+A">Allison Kirkpatrick</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="2309.05835v1-abstract-short" style="display: inline;"> Low mass (sub)stellar objects represent the low end of the initial mass function, the transition to free-floating planets and a prominent interloper population in the search for high-redshift galaxies. Without proper motions or spectroscopy, can one identify these objects photometrically? JWST/NIRCam has several advantages over HST/WFC3 NIR: more filters, a greater wavelength range, and greater sp… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.05835v1-abstract-full').style.display = 'inline'; document.getElementById('2309.05835v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.05835v1-abstract-full" style="display: none;"> Low mass (sub)stellar objects represent the low end of the initial mass function, the transition to free-floating planets and a prominent interloper population in the search for high-redshift galaxies. Without proper motions or spectroscopy, can one identify these objects photometrically? JWST/NIRCam has several advantages over HST/WFC3 NIR: more filters, a greater wavelength range, and greater spatial resolution. Here, we present a catalogue of (sub)stellar dwarfs identified in the Cosmic Evolution Early Release Science Survey (CEERS). We identify 518 stellar objects down to $m_F200W \sim 28$ using half-light radius, a full three magnitudes deeper than typical HST/WFC3 images. A kNN nearest neighbour algorithm identifies and types these sources, using four HST/WFC3 and four NIRCam filters, trained on SpeX spectra of nearby brown dwarfs. The kNN with four neighbors classifies well within two subtypes: e.g M2$\pm$2 or T4$\pm$2, achieving $\sim$95% precision and recall. More granular typing results in worse metrics. In CEERS, we find 9 M8$\pm$2, 2 L6$\pm$2, 1 T4$\pm$2, and 15 T8$\pm$2. We compare the observed long wavelength NIRCam colours -- not used in the kNN -- to those expected for brown dwarf atmospheric models. The NIRCam F356W-F444W and F410M-F444W colours are redder by a magnitude for the type assigned by the kNN, hinting at a wider variety of atmospheres for these objects. We find a 300-350pc scale-height for M6$\pm$2 dwarfs plus a second structural component and a 150-200pc scale-height for T6$\pm$2 type dwarfs, consistent with literature values. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.05835v1-abstract-full').style.display = 'none'; document.getElementById('2309.05835v1-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 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 24 figures, 3 tables, submitted 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/2203.15611">arXiv:2203.15611</a> <span> [<a href="https://arxiv.org/pdf/2203.15611">pdf</a>, <a href="https://arxiv.org/format/2203.15611">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stac889">10.1093/mnras/stac889 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxy And Mass Assembly (GAMA): Self-Organizing Map Application on Nearby Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B+W">B. W. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+D">Dominic Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Porter%2C+L">Lori Porter</a>, <a href="/search/astro-ph?searchtype=author&query=Henry%2C+C">Chris Henry</a>, <a href="/search/astro-ph?searchtype=author&query=Porter-Temple%2C+R">Ren Porter-Temple</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K">Kyle Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Pimbblet%2C+K+A">Kevin A. Pimbblet</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A+M">Andrew M. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Bilicki%2C+M">Maciej Bilicki</a>, <a href="/search/astro-ph?searchtype=author&query=Turner%2C+S">Sebastian Turner</a>, <a href="/search/astro-ph?searchtype=author&query=Acquaviva%2C+V">Viviana Acquaviva</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+L">Lingyu Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Wright%2C+A+H">Angus H. Wright</a>, <a href="/search/astro-ph?searchtype=author&query=Kelvin%2C+L+S">Lee S. Kelvin</a>, <a href="/search/astro-ph?searchtype=author&query=Grootes%2C+M+W">Meiert W. Grootes</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="2203.15611v1-abstract-short" style="display: inline;"> Galaxy populations show bimodality in a variety of properties: stellar mass, colour, specific star-formation rate, size, and S茅rsic index. These parameters are our feature space. We use an existing sample of 7556 galaxies from the Galaxy and Mass Assembly (GAMA) survey, represented using five features and the K-means clustering technique, showed that the bimodalities are the manifestation of a mor… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.15611v1-abstract-full').style.display = 'inline'; document.getElementById('2203.15611v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.15611v1-abstract-full" style="display: none;"> Galaxy populations show bimodality in a variety of properties: stellar mass, colour, specific star-formation rate, size, and S茅rsic index. These parameters are our feature space. We use an existing sample of 7556 galaxies from the Galaxy and Mass Assembly (GAMA) survey, represented using five features and the K-means clustering technique, showed that the bimodalities are the manifestation of a more complex population structure, represented by between 2 and 6 clusters. Here we use Self Organizing Maps (SOM), an unsupervised learning technique which can be used to visualize similarity in a higher dimensional space using a 2D representation, to map these five-dimensional clusters in the feature space onto two-dimensional projections. To further analyze these clusters, using the SOM information, we agree with previous results that the sub-populations found in the feature space can be reasonably mapped onto three or five clusters. We explore where the "green valley" galaxies are mapped onto the SOM, indicating multiple interstitial populations within the green valley population. Finally, we use the projection of the SOM to verify whether morphological information provided by GalaxyZoo users, for example, if features are visible, can be mapped onto the SOM-generated map. Voting on whether galaxies are smooth, likely ellipticals, or "featured" can reasonably be separated but smaller morphological features (bar, spiral arms) can not. SOMs promise to be a useful tool to map and identify instructive sub-populations in multidimensional galaxy survey feature space, provided they are large enough. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.15611v1-abstract-full').style.display = 'none'; document.getElementById('2203.15611v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 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">14 pages, 14 figures, accepted by MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1711.10621">arXiv:1711.10621</a> <span> [<a href="https://arxiv.org/pdf/1711.10621">pdf</a>, <a href="https://arxiv.org/format/1711.10621">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> <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/10.1016/j.icarus.2017.11.033">10.1016/j.icarus.2017.11.033 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Large Synoptic Survey Telescope as a Near-Earth Object Discovery Machine </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jones%2C+R+L">R. Lynne Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Slater%2C+C+T">Colin T. Slater</a>, <a href="/search/astro-ph?searchtype=author&query=Moeyens%2C+J">Joachim Moeyens</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+L">Lori Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Axelrod%2C+T">Tim Axelrod</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K">Kem Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Ivezi%C4%87%2C+%C5%BD">沤eljko Ivezi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Juri%C4%87%2C+M">Mario Juri膰</a>, <a href="/search/astro-ph?searchtype=author&query=Myers%2C+J">Jonathan Myers</a>, <a href="/search/astro-ph?searchtype=author&query=Petry%2C+C+E">Catherine E. Petry</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="1711.10621v1-abstract-short" style="display: inline;"> Using the most recent prototypes, design, and as-built system information, we test and quantify the capability of the Large Synoptic Survey Telescope (LSST) to discover Potentially Hazardous Asteroids (PHAs) and Near-Earth Objects (NEOs). We empirically estimate an expected upper limit to the false detection rate in LSST image differencing, using measurements on DECam data and prototype LSST softw… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1711.10621v1-abstract-full').style.display = 'inline'; document.getElementById('1711.10621v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1711.10621v1-abstract-full" style="display: none;"> Using the most recent prototypes, design, and as-built system information, we test and quantify the capability of the Large Synoptic Survey Telescope (LSST) to discover Potentially Hazardous Asteroids (PHAs) and Near-Earth Objects (NEOs). We empirically estimate an expected upper limit to the false detection rate in LSST image differencing, using measurements on DECam data and prototype LSST software and find it to be about $450$~deg$^{-2}$. We show that this rate is already tractable with current prototype of the LSST Moving Object Processing System (MOPS) by processing a 30-day simulation consistent with measured false detection rates. We proceed to evaluate the performance of the LSST baseline survey strategy for PHAs and NEOs using a high-fidelity simulated survey pointing history. We find that LSST alone, using its baseline survey strategy, will detect $66\%$ of the PHA and $61\%$ of the NEO population objects brighter than $H=22$, with the uncertainty in the estimate of $\pm5$ percentage points. By generating and examining variations on the baseline survey strategy, we show it is possible to further improve the discovery yields. In particular, we find that extending the LSST survey by two additional years and doubling the MOPS search window increases the completeness for PHAs to $86\%$ (including those discovered by contemporaneous surveys) without jeopardizing other LSST science goals ($77\%$ for NEOs). This equates to reducing the undiscovered population of PHAs by additional $26\%$ ($15\%$ for NEOs), relative to the baseline survey. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1711.10621v1-abstract-full').style.display = 'none'; document.getElementById('1711.10621v1-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 November, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">66 pages, 18 figures, accepted to Icarus</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1708.07909">arXiv:1708.07909</a> <span> [<a href="https://arxiv.org/pdf/1708.07909">pdf</a>, <a href="https://arxiv.org/format/1708.07909">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/10.1093/mnras/stx2221">10.1093/mnras/stx2221 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Investigating the physical properties of transiting hot Jupiters with the 1.5-m Kuiper Telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Turner%2C+J+D">Jake D. Turner</a>, <a href="/search/astro-ph?searchtype=author&query=Leiter%2C+R+M">Robin M. Leiter</a>, <a href="/search/astro-ph?searchtype=author&query=Biddle%2C+L+I">Lauren I. Biddle</a>, <a href="/search/astro-ph?searchtype=author&query=Pearson%2C+K+A">Kyle A. Pearson</a>, <a href="/search/astro-ph?searchtype=author&query=Hardegree-Ullman%2C+K+K">Kevin K. Hardegree-Ullman</a>, <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+R+M">Robert M. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Teske%2C+J+K">Johanna K. Teske</a>, <a href="/search/astro-ph?searchtype=author&query=Cates%2C+I+T">Ian T. Cates</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K+L">Kendall L. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Berube%2C+M+P">Michael P. Berube</a>, <a href="/search/astro-ph?searchtype=author&query=Nieberding%2C+M+N">Megan N. Nieberding</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+C+K">Christen K. Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Raphael%2C+B">Brandon Raphael</a>, <a href="/search/astro-ph?searchtype=author&query=Wallace%2C+S">Spencer Wallace</a>, <a href="/search/astro-ph?searchtype=author&query=Watson%2C+Z+T">Zachary T. Watson</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+R+E">Robert E. Johnson</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="1708.07909v1-abstract-short" style="display: inline;"> We present new photometric data of 11 hot Jupiter transiting exoplanets (CoRoT-12b, HAT-P-5b, HAT-P-12b, HAT-P-33b, HAT-P-37b, WASP-2b, WASP-24b, WASP-60b, WASP-80b, WASP-103b, XO-3b) in order to update their planetary parameters and to constrain information about their atmospheres. These observations of CoRoT-12b, HAT-P-37b and WASP-60b are the first follow-up data since their discovery. Addition… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1708.07909v1-abstract-full').style.display = 'inline'; document.getElementById('1708.07909v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1708.07909v1-abstract-full" style="display: none;"> We present new photometric data of 11 hot Jupiter transiting exoplanets (CoRoT-12b, HAT-P-5b, HAT-P-12b, HAT-P-33b, HAT-P-37b, WASP-2b, WASP-24b, WASP-60b, WASP-80b, WASP-103b, XO-3b) in order to update their planetary parameters and to constrain information about their atmospheres. These observations of CoRoT-12b, HAT-P-37b and WASP-60b are the first follow-up data since their discovery. Additionally, the first near-UV transits of WASP-80b and WASP-103b are presented. We compare the results of our analysis with previous work to search for transit timing variations (TTVs) and a wavelength dependence in the transit depth. TTVs may be evidence of a third body in the system and variations in planetary radius with wavelength can help constrain the properties of the exoplanet's atmosphere. For WASP-103b and XO-3b, we find a possible variation in the transit depths that may be evidence of scattering in their atmospheres. The B-band transit depth of HAT-P-37b is found to be smaller than its near-IR transit depth and such a variation may indicate TiO/VO absorption. These variations are detected from 2-4.6$蟽$, so follow-up observations are needed to confirm these results. Additionally, a flat spectrum across optical wavelengths is found for 5 of the planets (HAT-P-5b, HAT-P-12b, WASP-2b, WASP-24b, WASP-80b), suggestive that clouds may be present in their atmospheres. We calculate a refined orbital period and ephemeris for all the targets, which will help with future observations. No TTVs are seen in our analysis with the exception of WASP-80b and follow-up observations are needed to confirm this possible detection. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1708.07909v1-abstract-full').style.display = 'none'; document.getElementById('1708.07909v1-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 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">18 pages, 7 figures, 9 Tables. Light Curves available online. Accepted to MNRAS (2017 August 25)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1708.04058">arXiv:1708.04058</a> <span> [<a href="https://arxiv.org/pdf/1708.04058">pdf</a>, <a href="https://arxiv.org/format/1708.04058">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.5281/zenodo.842713">10.5281/zenodo.842713 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Science-Driven Optimization of the LSST Observing Strategy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=LSST+Science+Collaboration"> LSST Science Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+P">Phil Marshall</a>, <a href="/search/astro-ph?searchtype=author&query=Anguita%2C+T">Timo Anguita</a>, <a href="/search/astro-ph?searchtype=author&query=Bianco%2C+F+B">Federica B. Bianco</a>, <a href="/search/astro-ph?searchtype=author&query=Bellm%2C+E+C">Eric C. Bellm</a>, <a href="/search/astro-ph?searchtype=author&query=Brandt%2C+N">Niel Brandt</a>, <a href="/search/astro-ph?searchtype=author&query=Clarkson%2C+W">Will Clarkson</a>, <a href="/search/astro-ph?searchtype=author&query=Connolly%2C+A">Andy Connolly</a>, <a href="/search/astro-ph?searchtype=author&query=Gawiser%2C+E">Eric Gawiser</a>, <a href="/search/astro-ph?searchtype=author&query=Ivezic%2C+Z">Zeljko Ivezic</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+L">Lynne Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Lochner%2C+M">Michelle Lochner</a>, <a href="/search/astro-ph?searchtype=author&query=Lund%2C+M+B">Michael B. Lund</a>, <a href="/search/astro-ph?searchtype=author&query=Mahabal%2C+A">Ashish Mahabal</a>, <a href="/search/astro-ph?searchtype=author&query=Nidever%2C+D">David Nidever</a>, <a href="/search/astro-ph?searchtype=author&query=Olsen%2C+K">Knut Olsen</a>, <a href="/search/astro-ph?searchtype=author&query=Ridgway%2C+S">Stephen Ridgway</a>, <a href="/search/astro-ph?searchtype=author&query=Rhodes%2C+J">Jason Rhodes</a>, <a href="/search/astro-ph?searchtype=author&query=Shemmer%2C+O">Ohad Shemmer</a>, <a href="/search/astro-ph?searchtype=author&query=Trilling%2C+D">David Trilling</a>, <a href="/search/astro-ph?searchtype=author&query=Vivas%2C+K">Kathy Vivas</a>, <a href="/search/astro-ph?searchtype=author&query=Walkowicz%2C+L">Lucianne Walkowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Willman%2C+B">Beth Willman</a>, <a href="/search/astro-ph?searchtype=author&query=Yoachim%2C+P">Peter Yoachim</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+S">Scott Anderson</a> , et al. (80 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="1708.04058v1-abstract-short" style="display: inline;"> The Large Synoptic Survey Telescope is designed to provide an unprecedented optical imaging dataset that will support investigations of our Solar System, Galaxy and Universe, across half the sky and over ten years of repeated observation. However, exactly how the LSST observations will be taken (the observing strategy or "cadence") is not yet finalized. In this dynamically-evolving community white… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1708.04058v1-abstract-full').style.display = 'inline'; document.getElementById('1708.04058v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1708.04058v1-abstract-full" style="display: none;"> The Large Synoptic Survey Telescope is designed to provide an unprecedented optical imaging dataset that will support investigations of our Solar System, Galaxy and Universe, across half the sky and over ten years of repeated observation. However, exactly how the LSST observations will be taken (the observing strategy or "cadence") is not yet finalized. In this dynamically-evolving community white paper, we explore how the detailed performance of the anticipated science investigations is expected to depend on small changes to the LSST observing strategy. Using realistic simulations of the LSST schedule and observation properties, we design and compute diagnostic metrics and Figures of Merit that provide quantitative evaluations of different observing strategies, analyzing their impact on a wide range of proposed science projects. This is work in progress: we are using this white paper to communicate to each other the relative merits of the observing strategy choices that could be made, in an effort to maximize the scientific value of the survey. The investigation of some science cases leads to suggestions for new strategies that could be simulated and potentially adopted. Notably, we find motivation for exploring departures from a spatially uniform annual tiling of the sky: focusing instead on different parts of the survey area in different years in a "rolling cadence" is likely to have significant benefits for a number of time domain and moving object astronomy projects. The communal assembly of a suite of quantified and homogeneously coded metrics is the vital first step towards an automated, systematic, science-based assessment of any given cadence simulation, that will enable the scheduling of the LSST to be as well-informed as possible. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1708.04058v1-abstract-full').style.display = 'none'; document.getElementById('1708.04058v1-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, 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">312 pages, 90 figures. Browse the current version at https://github.com/LSSTScienceCollaborations/ObservingStrategy, new contributions welcome!</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1607.06195">arXiv:1607.06195</a> <span> [<a href="https://arxiv.org/pdf/1607.06195">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1038/nature16452">10.1038/nature16452 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Repetitive Patterns in Rapid Optical Variations in the Nearby Black-hole Binary V404 Cygni </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kimura%2C+M">Mariko Kimura</a>, <a href="/search/astro-ph?searchtype=author&query=Isogai%2C+K">Keisuke Isogai</a>, <a href="/search/astro-ph?searchtype=author&query=Kato%2C+T">Taichi Kato</a>, <a href="/search/astro-ph?searchtype=author&query=Ueda%2C+Y">Yoshihiro Ueda</a>, <a href="/search/astro-ph?searchtype=author&query=Nakahira%2C+S">Satoshi Nakahira</a>, <a href="/search/astro-ph?searchtype=author&query=Shidatsu%2C+M">Megumi Shidatsu</a>, <a href="/search/astro-ph?searchtype=author&query=Enoto%2C+T">Teruaki Enoto</a>, <a href="/search/astro-ph?searchtype=author&query=Hori%2C+T">Takafumi Hori</a>, <a href="/search/astro-ph?searchtype=author&query=Nogami%2C+D">Daisaku Nogami</a>, <a href="/search/astro-ph?searchtype=author&query=Littlefield%2C+C">Colin Littlefield</a>, <a href="/search/astro-ph?searchtype=author&query=Ishioka%2C+R">Ryoko Ishioka</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Y">Ying-Tung Chen</a>, <a href="/search/astro-ph?searchtype=author&query=King%2C+S">Sun-Kun King</a>, <a href="/search/astro-ph?searchtype=author&query=Wen%2C+C">Chih-Yi Wen</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+S">Shiang-Yu Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Lehner%2C+M+J">Matthew J. Lehner</a>, <a href="/search/astro-ph?searchtype=author&query=Schwamb%2C+M+E">Megan E. Schwamb</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+J">Jen-Hung Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+Z">Zhi-Wei Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Alcock%2C+C">Charles Alcock</a>, <a href="/search/astro-ph?searchtype=author&query=Axelrod%2C+T">Tim Axelrod</a>, <a href="/search/astro-ph?searchtype=author&query=Bianco%2C+F+B">Federica B. Bianco</a>, <a href="/search/astro-ph?searchtype=author&query=Byun%2C+Y">Yong-Ik Byun</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W">Wen-Ping Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K+H">Kem H. Cook</a> , et al. (43 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="1607.06195v1-abstract-short" style="display: inline;"> How black holes accrete surrounding matter is a fundamental, yet unsolved question in astrophysics. It is generally believed that matter is absorbed into black holes via accretion disks, the state of which depends primarily on the mass-accretion rate. When this rate approaches the critical rate (the Eddington limit), thermal instability is supposed to occur in the inner disc, causing repetitive pa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1607.06195v1-abstract-full').style.display = 'inline'; document.getElementById('1607.06195v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1607.06195v1-abstract-full" style="display: none;"> How black holes accrete surrounding matter is a fundamental, yet unsolved question in astrophysics. It is generally believed that matter is absorbed into black holes via accretion disks, the state of which depends primarily on the mass-accretion rate. When this rate approaches the critical rate (the Eddington limit), thermal instability is supposed to occur in the inner disc, causing repetitive patterns of large-amplitude X-ray variability (oscillations) on timescales of minutes to hours. In fact, such oscillations have been observed only in sources with a high mass accretion rate, such as GRS 1915+105. These large-amplitude, relatively slow timescale, phenomena are thought to have physical origins distinct from X-ray or optical variations with small amplitudes and fast ($\lesssim$10 sec) timescales often observed in other black hole binaries (e.g., XTE J1118+480 and GX 339-4). Here we report an extensive multi-colour optical photometric data set of V404 Cygni, an X-ray transient source containing a black hole of nine solar masses (and a conpanion star) at a distance of 2.4 kiloparsecs. Our data show that optical oscillations on timescales of 100 seconds to 2.5 hours can occur at mass-accretion rates more than ten times lower than previously thought. This suggests that the accretion rate is not the critical parameter for inducing inner-disc instabilities. Instead, we propose that a long orbital period is a key condition for these large-amplitude oscillations, because the outer part of the large disc in binaries with long orbital periods will have surface densities too low to maintain sustained mass accretion to the inner part of the disc. The lack of sustained accretion -- not the actual rate -- would then be the critical factor causing large-amplitude oscillations in long-period systems. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1607.06195v1-abstract-full').style.display = 'none'; document.getElementById('1607.06195v1-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 July, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published in Nature on January 7th, 2016</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nature, Volume 529, Issue 7584, pp. 54-58 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1603.02587">arXiv:1603.02587</a> <span> [<a href="https://arxiv.org/pdf/1603.02587">pdf</a>, <a href="https://arxiv.org/format/1603.02587">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/10.1093/mnras/stw574">10.1093/mnras/stw574 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Ground-based near-UV observations of 15 transiting exoplanets: Constraints on their atmospheres and no evidence for asymmetrical transits </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Turner%2C+J+D">Jake D. Turner</a>, <a href="/search/astro-ph?searchtype=author&query=Pearson%2C+K+A">Kyle A. Pearson</a>, <a href="/search/astro-ph?searchtype=author&query=Biddle%2C+L+I">Lauren I. Biddle</a>, <a href="/search/astro-ph?searchtype=author&query=Smart%2C+B+M">Brianna M. Smart</a>, <a href="/search/astro-ph?searchtype=author&query=Zellem%2C+R+T">Robert T. Zellem</a>, <a href="/search/astro-ph?searchtype=author&query=Teske%2C+J+K">Johanna K. Teske</a>, <a href="/search/astro-ph?searchtype=author&query=Hardegree-Ullman%2C+K+K">Kevin K. Hardegree-Ullman</a>, <a href="/search/astro-ph?searchtype=author&query=Griffith%2C+C+C">Caitlin C. Griffith</a>, <a href="/search/astro-ph?searchtype=author&query=Leiter%2C+R+M">Robin M. Leiter</a>, <a href="/search/astro-ph?searchtype=author&query=Cates%2C+I+T">Ian T. Cates</a>, <a href="/search/astro-ph?searchtype=author&query=Nieberding%2C+M+N">Megan N. Nieberding</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+C+W">Carter-Thaxton W. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+R+M">Robert M. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Hofmann%2C+R">Ryan Hofmann</a>, <a href="/search/astro-ph?searchtype=author&query=Berube%2C+M+P">Michael P. Berube</a>, <a href="/search/astro-ph?searchtype=author&query=Nguyen%2C+C+H">Chi H. Nguyen</a>, <a href="/search/astro-ph?searchtype=author&query=Small%2C+L+C">Lindsay C. Small</a>, <a href="/search/astro-ph?searchtype=author&query=Guvenen%2C+B+C">Blythe C. Guvenen</a>, <a href="/search/astro-ph?searchtype=author&query=Richardson%2C+L">Logan Richardson</a>, <a href="/search/astro-ph?searchtype=author&query=McGraw%2C+A">Allison McGraw</a>, <a href="/search/astro-ph?searchtype=author&query=Raphael%2C+B">Brandon Raphael</a>, <a href="/search/astro-ph?searchtype=author&query=Crawford%2C+B+E">Benjamin E. Crawford</a>, <a href="/search/astro-ph?searchtype=author&query=Robertson%2C+A+N">Amy N. Robertson</a>, <a href="/search/astro-ph?searchtype=author&query=Tombleson%2C+R">Ryan Tombleson</a>, <a href="/search/astro-ph?searchtype=author&query=Carleton%2C+T+M">Timothy M. Carleton</a> , et al. (15 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="1603.02587v1-abstract-short" style="display: inline;"> Transits of exoplanets observed in the near-UV have been used to study the scattering properties of their atmospheres and possible star-planet interactions. We observed the primary transits of 15 exoplanets (CoRoT-1b, GJ436b, HAT-P-1b, HAT-P-13b, HAT-P-16b, HAT-P-22b, TrES-2b, TrES-4b, WASP-1b, WASP-12b, WASP-33b, WASP-36b, WASP-44b, WASP-48b, and WASP-77Ab) in the near-UV and several optical phot… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1603.02587v1-abstract-full').style.display = 'inline'; document.getElementById('1603.02587v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1603.02587v1-abstract-full" style="display: none;"> Transits of exoplanets observed in the near-UV have been used to study the scattering properties of their atmospheres and possible star-planet interactions. We observed the primary transits of 15 exoplanets (CoRoT-1b, GJ436b, HAT-P-1b, HAT-P-13b, HAT-P-16b, HAT-P-22b, TrES-2b, TrES-4b, WASP-1b, WASP-12b, WASP-33b, WASP-36b, WASP-44b, WASP-48b, and WASP-77Ab) in the near-UV and several optical photometric bands to update their planetary parameters, ephemerides, search for a wavelength dependence in their transit depths to constrain their atmospheres, and determine if asymmetries are visible in their light curves. Here we present the first ground-based near-UV light curves for 12 of the targets (CoRoT-1b, GJ436b, HAT-P-1b, HAT-P-13b, HAT-P-22b, TrES-2b, TrES-4b, WASP-1b, WASP-33b, WASP-36b, WASP-48b, and WASP-77Ab). We find that none of the near-UV transits exhibit any non-spherical asymmetries, this result is consistent with recent theoretical predictions by Ben-Jaffel et al. and Turner et al. The multi-wavelength photometry indicates a constant transit depth from near-UV to optical wavelengths in 10 targets (suggestive of clouds), and a varying transit depth with wavelength in 5 targets (hinting at Rayleigh or aerosol scattering in their atmospheres). We also present the first detection of a smaller near-UV transit depth than that measured in the optical in WASP-1b and a possible opacity source that can cause such radius variations is currently unknown. WASP-36b also exhibits a smaller near-UV transit depth at 2.6$蟽$. Further observations are encouraged to confirm the transit depth variations seen in this study. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1603.02587v1-abstract-full').style.display = 'none'; document.getElementById('1603.02587v1-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 March, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">35 pages, 16 tables, 10 figures. Accepted for publication in MNRAS (March 8, 2016). Light curves are available online. Updated EXOMOP (transit modeling software) and is also available online</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1301.6182">arXiv:1301.6182</a> <span> [<a href="https://arxiv.org/pdf/1301.6182">pdf</a>, <a href="https://arxiv.org/ps/1301.6182">ps</a>, <a href="https://arxiv.org/format/1301.6182">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-6256/146/1/14">10.1088/0004-6256/146/1/14 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The TAOS Project: Results From Seven Years of Survey Data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+Z+-">Z. -W. Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Lehner%2C+M+J">M. J. Lehner</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+J+-">J. -H. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Wen%2C+C+-">C. -Y. Wen</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+S+-">S. -Y. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=King%2C+S+-">S. -K. King</a>, <a href="/search/astro-ph?searchtype=author&query=Granados%2C+%C3%81+P">脕. P. Granados</a>, <a href="/search/astro-ph?searchtype=author&query=Alcock%2C+C">C. Alcock</a>, <a href="/search/astro-ph?searchtype=author&query=Axelrod%2C+T">T. Axelrod</a>, <a href="/search/astro-ph?searchtype=author&query=Bianco%2C+F+B">F. B. Bianco</a>, <a href="/search/astro-ph?searchtype=author&query=Byun%2C+Y+-">Y. -I. Byun</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W+P">W. P. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Coehlo%2C+N+K">N. K. Coehlo</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K+H">K. H. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=de+Pater%2C+I">I. de Pater</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D+-">D. -W. Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+T">T. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lissauer%2C+J+J">J. J. Lissauer</a>, <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+S+L">S. L. Marshall</a>, <a href="/search/astro-ph?searchtype=author&query=Protopapas%2C+P">P. Protopapas</a>, <a href="/search/astro-ph?searchtype=author&query=Rice%2C+J+A">J. A. Rice</a>, <a href="/search/astro-ph?searchtype=author&query=Schwamb%2C+M+E">M. E. Schwamb</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1301.6182v1-abstract-short" style="display: inline;"> The Taiwanese-American Occultation Survey (TAOS) aims to detect serendipitous occultations of stars by small (about 1 km diameter) objects in the Kuiper Belt and beyond. Such events are very rare (<0.001 events per star per year) and short in duration (about 200 ms), so many stars must be monitored at a high readout cadence. TAOS monitors typically around 500 stars simultaneously at a 5 Hz readout… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1301.6182v1-abstract-full').style.display = 'inline'; document.getElementById('1301.6182v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1301.6182v1-abstract-full" style="display: none;"> The Taiwanese-American Occultation Survey (TAOS) aims to detect serendipitous occultations of stars by small (about 1 km diameter) objects in the Kuiper Belt and beyond. Such events are very rare (<0.001 events per star per year) and short in duration (about 200 ms), so many stars must be monitored at a high readout cadence. TAOS monitors typically around 500 stars simultaneously at a 5 Hz readout cadence with four telescopes located at Lulin Observatory in central Taiwan. In this paper, we report the results of the search for small Kuiper Belt Objects (KBOs) in seven years of data. No occultation events were found, resulting in a 95% c.l. upper limit on the slope of the faint end of the KBO size distribution of q = 3.34 to 3.82, depending on the surface density at the break in the size distribution at a diameter of about 90 km. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1301.6182v1-abstract-full').style.display = 'none'; document.getElementById('1301.6182v1-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 January, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 9 figures. Submitted to Astronomical Journal 2013 January 16</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1211.2608">arXiv:1211.2608</a> <span> [<a href="https://arxiv.org/pdf/1211.2608">pdf</a>, <a href="https://arxiv.org/ps/1211.2608">ps</a>, <a href="https://arxiv.org/format/1211.2608">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201220714">10.1051/0004-6361/201220714 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Simultaneous Low State Spectral Energy Distribution of 1ES 2344+514 from Radio to Very High Energies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=MAGIC+Collaboration"> MAGIC Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Aleksi%C4%87%2C+J">J. Aleksi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Antoranz%2C+P">P. Antoranz</a>, <a href="/search/astro-ph?searchtype=author&query=Asensio%2C+M">M. Asensio</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=de+Almeida%2C+U+B">U. Barres de Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Barrio%2C+J+A">J. A. Barrio</a>, <a href="/search/astro-ph?searchtype=author&query=Bednarek%2C+W">W. Bednarek</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+K">K. Berger</a>, <a href="/search/astro-ph?searchtype=author&query=Bernardini%2C+E">E. Bernardini</a>, <a href="/search/astro-ph?searchtype=author&query=Biland%2C+A">A. Biland</a>, <a href="/search/astro-ph?searchtype=author&query=Blanch%2C+O">O. Blanch</a>, <a href="/search/astro-ph?searchtype=author&query=Bock%2C+R+K">R. K. Bock</a>, <a href="/search/astro-ph?searchtype=author&query=Boller%2C+A">A. Boller</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnefoy%2C+S">S. Bonnefoy</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnoli%2C+G">G. Bonnoli</a>, <a href="/search/astro-ph?searchtype=author&query=Tridon%2C+D+B">D. Borla Tridon</a>, <a href="/search/astro-ph?searchtype=author&query=Bretz%2C+T">T. Bretz</a>, <a href="/search/astro-ph?searchtype=author&query=Carmona%2C+E">E. Carmona</a>, <a href="/search/astro-ph?searchtype=author&query=Carosi%2C+A">A. Carosi</a>, <a href="/search/astro-ph?searchtype=author&query=Fidalgo%2C+D+C">D. Carreto Fidalgo</a>, <a href="/search/astro-ph?searchtype=author&query=Colin%2C+P">P. Colin</a>, <a href="/search/astro-ph?searchtype=author&query=Colombo%2C+E">E. Colombo</a>, <a href="/search/astro-ph?searchtype=author&query=Contreras%2C+J+L">J. L. Contreras</a> , et al. (169 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="1211.2608v2-abstract-short" style="display: inline;"> [Abridged] Context. To construct and interpret the spectral energy distribution (SED) of BL Lacertae objects, simultaneous broad-band observations are mandatory. Aims. We present the results of a dedicated multi-wavelength study of the high-frequency peaked BL Lacertae (HBL) object and known TeV emitter 1ES 2344+514 by means of a pre-organised campaign. Methods. The observations were conducted dur… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1211.2608v2-abstract-full').style.display = 'inline'; document.getElementById('1211.2608v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1211.2608v2-abstract-full" style="display: none;"> [Abridged] Context. To construct and interpret the spectral energy distribution (SED) of BL Lacertae objects, simultaneous broad-band observations are mandatory. Aims. We present the results of a dedicated multi-wavelength study of the high-frequency peaked BL Lacertae (HBL) object and known TeV emitter 1ES 2344+514 by means of a pre-organised campaign. Methods. The observations were conducted during simultaneous visibility windows of MAGIC and AGILE in late 2008. The measurements were complemented by Mets盲hovi, RATAN-600, KVA+Tuorla, Swift and VLBA pointings. Additional coverage was provided by the ongoing long-term F-GAMMA and MOJAVE programs, the OVRO 40-m and CrAO telescopes as well as the Fermi satellite. The obtained SEDs are modelled using a one-zone as well as a self-consistent two-zone synchrotron self-Compton model. Results. 1ES 2344+514 was found at very low flux states in both X-rays and very high energy gamma rays. Variability was detected in the low frequency radio and X-ray bands only, where for the latter a small flare was observed. The X-ray flare was possibly caused by shock acceleration characterised by similar cooling and acceleration time scales. MOJAVE VLBA monitoring reveals a static jet whose components are stable over time scales of eleven years, contrary to previous findings. There appears to be no significant correlation between the 15 GHz and R-band monitoring light curves. The observations presented here constitute the first multi-wavelength campaign on 1ES 2344+514 from radio to VHE energies and one of the few simultaneous SEDs during low activity states. The quasi-simultaneous Fermi-LAT data poses some challenges for SED modelling, but in general the SEDs are described well by both applied models. The resulting parameters are typical for TeV emitting HBLs. Consequently it remains unclear whether a so-called quiescent state was found in this campaign. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1211.2608v2-abstract-full').style.display = 'none'; document.getElementById('1211.2608v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 June, 2013; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 November, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">29 pages, 20 figures, 10 tables, accepted for publication by A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1208.4012">arXiv:1208.4012</a> <span> [<a href="https://arxiv.org/pdf/1208.4012">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"> Wide-Field InfraRed Survey Telescope (WFIRST) Final Report </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Green%2C+J">J. Green</a>, <a href="/search/astro-ph?searchtype=author&query=Schechter%2C+P">P. Schechter</a>, <a href="/search/astro-ph?searchtype=author&query=Baltay%2C+C">C. Baltay</a>, <a href="/search/astro-ph?searchtype=author&query=Bean%2C+R">R. Bean</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+D">D. Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+R">R. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C">C. Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=Donahue%2C+M">M. Donahue</a>, <a href="/search/astro-ph?searchtype=author&query=Fan%2C+X">X. Fan</a>, <a href="/search/astro-ph?searchtype=author&query=Gaudi%2C+B+S">B. S. Gaudi</a>, <a href="/search/astro-ph?searchtype=author&query=Hirata%2C+C">C. Hirata</a>, <a href="/search/astro-ph?searchtype=author&query=Kalirai%2C+J">J. Kalirai</a>, <a href="/search/astro-ph?searchtype=author&query=Lauer%2C+T">T. Lauer</a>, <a href="/search/astro-ph?searchtype=author&query=Nichol%2C+B">B. Nichol</a>, <a href="/search/astro-ph?searchtype=author&query=Padmanabhan%2C+N">N. Padmanabhan</a>, <a href="/search/astro-ph?searchtype=author&query=Perlmutter%2C+S">S. Perlmutter</a>, <a href="/search/astro-ph?searchtype=author&query=Rauscher%2C+B">B. Rauscher</a>, <a href="/search/astro-ph?searchtype=author&query=Rhodes%2C+J">J. Rhodes</a>, <a href="/search/astro-ph?searchtype=author&query=Roellig%2C+T">T. Roellig</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">D. Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Sumi%2C+T">T. Sumi</a>, <a href="/search/astro-ph?searchtype=author&query=Tanner%2C+A">A. Tanner</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Y">Y. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Weinberg%2C+D">D. Weinberg</a>, <a href="/search/astro-ph?searchtype=author&query=Wright%2C+E">E. Wright</a> , et al. (29 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1208.4012v1-abstract-short" style="display: inline;"> In December 2010, NASA created a Science Definition Team (SDT) for WFIRST, the Wide Field Infra-Red Survey Telescope, recommended by the Astro 2010 Decadal Survey as the highest priority for a large space mission. The SDT was chartered to work with the WFIRST Project Office at GSFC and the Program Office at JPL to produce a Design Reference Mission (DRM) for WFIRST. Part of the original charge was… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1208.4012v1-abstract-full').style.display = 'inline'; document.getElementById('1208.4012v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1208.4012v1-abstract-full" style="display: none;"> In December 2010, NASA created a Science Definition Team (SDT) for WFIRST, the Wide Field Infra-Red Survey Telescope, recommended by the Astro 2010 Decadal Survey as the highest priority for a large space mission. The SDT was chartered to work with the WFIRST Project Office at GSFC and the Program Office at JPL to produce a Design Reference Mission (DRM) for WFIRST. Part of the original charge was to produce an interim design reference mission by mid-2011. That document was delivered to NASA and widely circulated within the astronomical community. In late 2011 the Astrophysics Division augmented its original charge, asking for two design reference missions. The first of these, DRM1, was to be a finalized version of the interim DRM, reducing overall mission costs where possible. The second of these, DRM2, was to identify and eliminate capabilities that overlapped with those of NASA's James Webb Space Telescope (henceforth JWST), ESA's Euclid mission, and the NSF's ground-based Large Synoptic Survey Telescope (henceforth LSST), and again to reduce overall mission cost, while staying faithful to NWNH. This report presents both DRM1 and DRM2. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1208.4012v1-abstract-full').style.display = 'none'; document.getElementById('1208.4012v1-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 August, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">102 pages, 57 figures, 17 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/1208.2323">arXiv:1208.2323</a> <span> [<a href="https://arxiv.org/pdf/1208.2323">pdf</a>, <a href="https://arxiv.org/ps/1208.2323">ps</a>, <a href="https://arxiv.org/format/1208.2323">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/760/2/116">10.1088/0004-637X/760/2/116 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Microlensig Binaries with Candidate Brown Dwarf Companions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I+-">I. -G. Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">C. Han</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">A. Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">A. Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Sumi%2C+T">T. Sumi</a>, <a href="/search/astro-ph?searchtype=author&query=Dominik%2C+M">M. Dominik</a>, <a href="/search/astro-ph?searchtype=author&query=Beaulieu%2C+J+-">J. -P. Beaulieu</a>, <a href="/search/astro-ph?searchtype=author&query=Tsapras%2C+Y">Y. Tsapras</a>, <a href="/search/astro-ph?searchtype=author&query=Bozza%2C+V">V. Bozza</a>, <a href="/search/astro-ph?searchtype=author&query=Szyma%C5%84ski%2C+M+K">M. K. Szyma艅ski</a>, <a href="/search/astro-ph?searchtype=author&query=Kubiak%2C+M">M. Kubiak</a>, <a href="/search/astro-ph?searchtype=author&query=Soszy%C5%84ski%2C+I">I. Soszy艅ski</a>, <a href="/search/astro-ph?searchtype=author&query=Pietrzy%C5%84ski%2C+G">G. Pietrzy艅ski</a>, <a href="/search/astro-ph?searchtype=author&query=Poleski%2C+R">R. Poleski</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">K. Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Pietrukowicz%2C+P">P. Pietrukowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Koz%C5%82owski%2C+S">S. Koz艂owski</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+J">J. Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Wyrzykowski%2C+%C5%81">艁. Wyrzykowski</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+F">F. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+D+P">D. P. Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+I+A">I. A. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Botzler%2C+C+S">C. S. Botzler</a>, <a href="/search/astro-ph?searchtype=author&query=Freeman%2C+M">M. Freeman</a>, <a href="/search/astro-ph?searchtype=author&query=Fukui%2C+A">A. Fukui</a> , et al. (130 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="1208.2323v2-abstract-short" style="display: inline;"> Brown dwarfs are important objects because they may provide a missing link between stars and planets, two populations that have dramatically different formation history. In this paper, we present the candidate binaries with brown dwarf companions that are found by analyzing binary microlensing events discovered during 2004 - 2011 observation seasons. Based on the low mass ratio criterion of q < 0.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1208.2323v2-abstract-full').style.display = 'inline'; document.getElementById('1208.2323v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1208.2323v2-abstract-full" style="display: none;"> Brown dwarfs are important objects because they may provide a missing link between stars and planets, two populations that have dramatically different formation history. In this paper, we present the candidate binaries with brown dwarf companions that are found by analyzing binary microlensing events discovered during 2004 - 2011 observation seasons. Based on the low mass ratio criterion of q < 0.2, we found 7 candidate events, including OGLE-2004-BLG-035, OGLE-2004-BLG-039, OGLE-2007-BLG-006, OGLE-2007-BLG-399/MOA-2007-BLG-334, MOA-2011-BLG-104/OGLE-2011-BLG-0172, MOA-2011-BLG-149, and MOA-201-BLG-278/OGLE-2011-BLG-012N. Among them, we are able to confirm that the companions of the lenses of MOA-2011-BLG-104/OGLE-2011-BLG-0172 and MOA-2011-BLG-149 are brown dwarfs by determining the mass of the lens based on the simultaneous measurement of the Einstein radius and the lens parallax. The measured mass of the brown dwarf companions are (0.02 +/- 0.01) M_Sun and (0.019 +/- 0.002) M_Sun for MOA-2011-BLG-104/OGLE-2011-BLG-0172 and MOA-2011-BLG-149, respectively, and both companions are orbiting low mass M dwarf host stars. More microlensing brown dwarfs are expected to be detected as the number of lensing events with well covered light curves increases with new generation searches. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1208.2323v2-abstract-full').style.display = 'none'; document.getElementById('1208.2323v2-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 October, 2012; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 August, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 9 figures, 4 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1207.1244">arXiv:1207.1244</a> <span> [<a href="https://arxiv.org/pdf/1207.1244">pdf</a>, <a href="https://arxiv.org/ps/1207.1244">ps</a>, <a href="https://arxiv.org/format/1207.1244">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/752/2/82">10.1088/0004-637X/752/2/82 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A possible binary system of a stellar remnant in the high magnification gravitational microlensing event OGLE-2007-BLG-514 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Miyake%2C+N">N. Miyake</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">A. Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Sumi%2C+T">T. Sumi</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+D+P">D. P. Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+S">S. Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Street%2C+R+A">R. A. Street</a>, <a href="/search/astro-ph?searchtype=author&query=Greenhill%2C+J">J. Greenhill</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+I+A">I. A. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">A. Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Kubiak%2C+M">M. Kubiak</a>, <a href="/search/astro-ph?searchtype=author&query=Szymanski%2C+M+K">M. K. Szymanski</a>, <a href="/search/astro-ph?searchtype=author&query=Pietrzynski%2C+G">G. Pietrzynski</a>, <a href="/search/astro-ph?searchtype=author&query=Soszynski%2C+I">I. Soszynski</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">K. Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Wyrzykowski%2C+L">L. Wyrzykowski</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+F">F. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Fukui%2C+A">A. Fukui</a>, <a href="/search/astro-ph?searchtype=author&query=Furusawa%2C+K">K. Furusawa</a>, <a href="/search/astro-ph?searchtype=author&query=Holderness%2C+S">S. Holderness</a>, <a href="/search/astro-ph?searchtype=author&query=Itow%2C+Y">Y. Itow</a>, <a href="/search/astro-ph?searchtype=author&query=Korpela%2C+A">A. Korpela</a>, <a href="/search/astro-ph?searchtype=author&query=Ling%2C+C+H">C. H. Ling</a>, <a href="/search/astro-ph?searchtype=author&query=Masuda%2C+K">K. Masuda</a>, <a href="/search/astro-ph?searchtype=author&query=Matsubara%2C+Y">Y. Matsubara</a>, <a href="/search/astro-ph?searchtype=author&query=Muraki%2C+Y">Y. Muraki</a> , et al. (56 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="1207.1244v1-abstract-short" style="display: inline;"> We report the extremely high magnification (A > 1000) binary microlensing event OGLE-2007-BLG-514. We obtained good coverage around the double peak structure in the light curve via follow-up observations from different observatories. The binary lens model that includes the effects of parallax (known orbital motion of the Earth) and orbital motion of the lens yields a binary lens mass ratio of q =… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1207.1244v1-abstract-full').style.display = 'inline'; document.getElementById('1207.1244v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1207.1244v1-abstract-full" style="display: none;"> We report the extremely high magnification (A > 1000) binary microlensing event OGLE-2007-BLG-514. We obtained good coverage around the double peak structure in the light curve via follow-up observations from different observatories. The binary lens model that includes the effects of parallax (known orbital motion of the Earth) and orbital motion of the lens yields a binary lens mass ratio of q = 0.321 +/- 0.007 and a projected separation of s = 0.072 +/- 0.001$ in units of the Einstein radius. The parallax parameters allow us to determine the lens distance D_L = 3.11 +/- 0.39 kpc and total mass M_L=1.40 +/- 0.18 M_sun; this leads to the primary and secondary components having masses of M_1 = 1.06 +/- 0.13 M_sun and M_2 = 0.34 +/- 0.04 M_sun, respectively. The parallax model indicates that the binary lens system is likely constructed by the main sequence stars. On the other hand, we used a Bayesian analysis to estimate probability distributions by the model that includes the effects of xallarap (possible orbital motion of the source around a companion) and parallax (q = 0.270 +/- 0.005, s = 0.083 +/- 0.001). The primary component of the binary lens is relatively massive with M_1 = 0.9_{-0.3}^{+4.6} M_sun and it is at a distance of D_L = 2.6_{-0.9}^{+3.8} kpc. Given the secure mass ratio measurement, the companion mass is therefore M_2 = 0.2_{-0.1}^{+1.2} M_sun. The xallarap model implies that the primary lens is likely a stellar remnant, such as a white dwarf, a neutron star or a black hole. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1207.1244v1-abstract-full').style.display = 'none'; document.getElementById('1207.1244v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 July, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">31 pages, 6 figures, 7 tables, accepted in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1203.1291">arXiv:1203.1291</a> <span> [<a href="https://arxiv.org/pdf/1203.1291">pdf</a>, <a href="https://arxiv.org/ps/1203.1291">ps</a>, <a href="https://arxiv.org/format/1203.1291">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> <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/10.1111/j.1365-2966.2012.21233.x">10.1111/j.1365-2966.2012.21233.x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> OGLE-2008-BLG-510: first automated real-time detection of a weak microlensing anomaly - brown dwarf or stellar binary? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bozza%2C+V">V. Bozza</a>, <a href="/search/astro-ph?searchtype=author&query=Dominik%2C+M">M. Dominik</a>, <a href="/search/astro-ph?searchtype=author&query=Rattenbury%2C+N+J">N. J. Rattenbury</a>, <a href="/search/astro-ph?searchtype=author&query=Joergensen%2C+U+G">U. G. Joergensen</a>, <a href="/search/astro-ph?searchtype=author&query=Tsapras%2C+Y">Y. Tsapras</a>, <a href="/search/astro-ph?searchtype=author&query=Bramich%2C+D+M">D. M. Bramich</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">A. Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+I+A">I. A. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Liebig%2C+C">C. Liebig</a>, <a href="/search/astro-ph?searchtype=author&query=Cassan%2C+A">A. Cassan</a>, <a href="/search/astro-ph?searchtype=author&query=Fouque%2C+P">P. Fouque</a>, <a href="/search/astro-ph?searchtype=author&query=Fukui%2C+A">A. Fukui</a>, <a href="/search/astro-ph?searchtype=author&query=Hundertmark%2C+M">M. Hundertmark</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I+-">I. -G. Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+S+H">S. H. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Choi%2C+J+-">J. -Y. Choi</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+S+-">S. -Y. Park</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">A. Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Allan%2C+A">A. Allan</a>, <a href="/search/astro-ph?searchtype=author&query=Mao%2C+S">S. Mao</a>, <a href="/search/astro-ph?searchtype=author&query=Wyrzykowski%2C+L">L. Wyrzykowski</a>, <a href="/search/astro-ph?searchtype=author&query=Street%2C+R+A">R. A. Street</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+D">D. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Nagayama%2C+T">T. Nagayama</a>, <a href="/search/astro-ph?searchtype=author&query=Mathiasen%2C+M">M. Mathiasen</a> , et al. (81 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="1203.1291v1-abstract-short" style="display: inline;"> The microlensing event OGLE-2008-BLG-510 is characterised by an evident asymmetric shape of the peak, promptly detected by the ARTEMiS system in real time. The skewness of the light curve appears to be compatible both with binary-lens and binary-source models, including the possibility that the lens system consists of an M dwarf orbited by a brown dwarf. The detection of this microlensing anomaly… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1203.1291v1-abstract-full').style.display = 'inline'; document.getElementById('1203.1291v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1203.1291v1-abstract-full" style="display: none;"> The microlensing event OGLE-2008-BLG-510 is characterised by an evident asymmetric shape of the peak, promptly detected by the ARTEMiS system in real time. The skewness of the light curve appears to be compatible both with binary-lens and binary-source models, including the possibility that the lens system consists of an M dwarf orbited by a brown dwarf. The detection of this microlensing anomaly and our analysis demonstrates that: 1) automated real-time detection of weak microlensing anomalies with immediate feedback is feasible, efficient, and sensitive, 2) rather common weak features intrinsically come with ambiguities that are not easily resolved from photometric light curves, 3) a modelling approach that finds all features of parameter space rather than just the `favourite model' is required, and 4) the data quality is most crucial, where systematics can be confused with real features, in particular small higher-order effects such as orbital motion signatures. It moreover becomes apparent that events with weak signatures are a silver mine for statistical studies, although not easy to exploit. Clues about the apparent paucity of both brown-dwarf companions and binary-source microlensing events might hide here. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1203.1291v1-abstract-full').style.display = 'none'; document.getElementById('1203.1291v1-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 March, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages with 8 figures, MNRAS submitted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1202.0903">arXiv:1202.0903</a> <span> [<a href="https://arxiv.org/pdf/1202.0903">pdf</a>, <a href="https://arxiv.org/format/1202.0903">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/10.1038/nature10684">10.1038/nature10684 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> One or more bound planets per Milky Way star from microlensing observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cassan%2C+A">A. Cassan</a>, <a href="/search/astro-ph?searchtype=author&query=Kubas%2C+D">D. Kubas</a>, <a href="/search/astro-ph?searchtype=author&query=Beaulieu%2C+J+-">J. -P. Beaulieu</a>, <a href="/search/astro-ph?searchtype=author&query=Dominik%2C+M">M. Dominik</a>, <a href="/search/astro-ph?searchtype=author&query=Horne%2C+K">K. Horne</a>, <a href="/search/astro-ph?searchtype=author&query=Greenhill%2C+J">J. Greenhill</a>, <a href="/search/astro-ph?searchtype=author&query=Wambsganss%2C+J">J. Wambsganss</a>, <a href="/search/astro-ph?searchtype=author&query=Menzies%2C+J">J. Menzies</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+A">A. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Jorgensen%2C+U+G">U. G. Jorgensen</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">A. Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+D+P">D. P. Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">M. D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+V">V. Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Brillant%2C+S">S. Brillant</a>, <a href="/search/astro-ph?searchtype=author&query=Caldwell%2C+J+A+R">J. A. R. Caldwell</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+A">A. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Coutures%2C+C">Ch. Coutures</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K+H">K. H. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Dieters%2C+S">S. Dieters</a>, <a href="/search/astro-ph?searchtype=author&query=Prester%2C+D+D">D. Dominis Prester</a>, <a href="/search/astro-ph?searchtype=author&query=Donatowicz%2C+J">J. Donatowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Fouque%2C+P">P. Fouque</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+K">K. Hill</a>, <a href="/search/astro-ph?searchtype=author&query=Kains%2C+N">N. Kains</a> , et al. (17 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1202.0903v1-abstract-short" style="display: inline;"> Most known extrasolar planets (exoplanets) have been discovered using the radial velocity$^{\bf 1,2}$ or transit$^{\bf 3}$ methods. Both are biased towards planets that are relatively close to their parent stars, and studies find that around 17--30% (refs 4, 5) of solar-like stars host a planet. Gravitational microlensing$^{\bf 6\rm{\bf -}\bf 9}$, on the other hand, probes planets that are further… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1202.0903v1-abstract-full').style.display = 'inline'; document.getElementById('1202.0903v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1202.0903v1-abstract-full" style="display: none;"> Most known extrasolar planets (exoplanets) have been discovered using the radial velocity$^{\bf 1,2}$ or transit$^{\bf 3}$ methods. Both are biased towards planets that are relatively close to their parent stars, and studies find that around 17--30% (refs 4, 5) of solar-like stars host a planet. Gravitational microlensing$^{\bf 6\rm{\bf -}\bf 9}$, on the other hand, probes planets that are further away from their stars. Recently, a population of planets that are unbound or very far from their stars was discovered by microlensing$^{\bf 10}$. These planets are at least as numerous as the stars in the Milky Way$^{\bf 10}$. Here we report a statistical analysis of microlensing data (gathered in 2002--07) that reveals the fraction of bound planets 0.5--10 AU (Sun--Earth distance) from their stars. We find that 17$_{\bf -9}^{\bf +6}$% of stars host Jupiter-mass planets (0.3--10 $\MJ$, where $\MJ {\bf = 318}$ $\Mearth$ and $\Mearth$ is Earth's mass). Cool Neptunes (10--30 $\Mearth$) and super-Earths (5--10 $\Mearth$) are even more common: their respective abundances per star are 52$_{\bf -29}^{\bf +22}$% and 62$_{\bf -37}^{\bf +35}$%. We conclude that stars are orbited by planets as a rule, rather than the exception. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1202.0903v1-abstract-full').style.display = 'none'; document.getElementById('1202.0903v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 February, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Letter, 2 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nature 481, 167-169 (2012) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1109.3295">arXiv:1109.3295</a> <span> [<a href="https://arxiv.org/pdf/1109.3295">pdf</a>, <a href="https://arxiv.org/ps/1109.3295">ps</a>, <a href="https://arxiv.org/format/1109.3295">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/746/2/127">10.1088/0004-637X/746/2/127 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Microlensing Binaries Discovered through High-Magnification Channel </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I+-">I. -G. Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Choi%2C+J+-">J. -Y. Choi</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+S+-">S. -Y. Park</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">C. Han</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">A. Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Sumi%2C+T">T. Sumi</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">A. Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Beaulieu%2C+J+-">J. -P. Beaulieu</a>, <a href="/search/astro-ph?searchtype=author&query=Dominik%2C+M">M. Dominik</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+W">W. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Bos%2C+M">M. Bos</a>, <a href="/search/astro-ph?searchtype=author&query=Christie%2C+G+W">G. W. Christie</a>, <a href="/search/astro-ph?searchtype=author&query=Depoy%2C+D+L">D. L. Depoy</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+S">S. Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Drummond%2C+J">J. Drummond</a>, <a href="/search/astro-ph?searchtype=author&query=Gal-Yam%2C+A">A. Gal-Yam</a>, <a href="/search/astro-ph?searchtype=author&query=Gaudi%2C+B+S">B. S. Gaudi</a>, <a href="/search/astro-ph?searchtype=author&query=Hung%2C+L+-">L. -W. Hung</a>, <a href="/search/astro-ph?searchtype=author&query=Janczak%2C+J">J. Janczak</a>, <a href="/search/astro-ph?searchtype=author&query=Kaspi%2C+S">S. Kaspi</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C+-">C. -U. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Mallia%2C+F">F. Mallia</a>, <a href="/search/astro-ph?searchtype=author&query=Maoz%2C+D">D. Maoz</a>, <a href="/search/astro-ph?searchtype=author&query=Maury%2C+A">A. Maury</a>, <a href="/search/astro-ph?searchtype=author&query=McCormick%2C+J">J. McCormick</a> , et al. (127 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="1109.3295v2-abstract-short" style="display: inline;"> Microlensing can provide a useful tool to probe binary distributions down to low-mass limits of binary companions. In this paper, we analyze the light curves of 8 binary lensing events detected through the channel of high-magnification events during the seasons from 2007 to 2010. The perturbations, which are confined near the peak of the light curves, can be easily distinguished from the central p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1109.3295v2-abstract-full').style.display = 'inline'; document.getElementById('1109.3295v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1109.3295v2-abstract-full" style="display: none;"> Microlensing can provide a useful tool to probe binary distributions down to low-mass limits of binary companions. In this paper, we analyze the light curves of 8 binary lensing events detected through the channel of high-magnification events during the seasons from 2007 to 2010. The perturbations, which are confined near the peak of the light curves, can be easily distinguished from the central perturbations caused by planets. However, the degeneracy between close and wide binary solutions cannot be resolved with a $3蟽$ confidence level for 3 events, implying that the degeneracy would be an important obstacle in studying binary distributions. The dependence of the degeneracy on the lensing parameters is consistent with a theoretic prediction that the degeneracy becomes severe as the binary separation and the mass ratio deviate from the values of resonant caustics. The measured mass ratio of the event OGLE-2008-BLG-510/MOA-2008-BLG-369 is $q\sim 0.1$, making the companion of the lens a strong brown-dwarf candidate. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1109.3295v2-abstract-full').style.display = 'none'; document.getElementById('1109.3295v2-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 November, 2011; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 September, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">10 figures, 6 tables, 26 pages</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1106.1210">arXiv:1106.1210</a> <span> [<a href="https://arxiv.org/pdf/1106.1210">pdf</a>, <a href="https://arxiv.org/ps/1106.1210">ps</a>, <a href="https://arxiv.org/format/1106.1210">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/738/1/25">10.1088/0004-637X/738/1/25 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> TeV and Multi-wavelength Observations of Mrk 421 in 2006-2008 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Acciari%2C+V+A">V. A. Acciari</a>, <a href="/search/astro-ph?searchtype=author&query=Aliu%2C+E">E. Aliu</a>, <a href="/search/astro-ph?searchtype=author&query=Arlen%2C+T">T. Arlen</a>, <a href="/search/astro-ph?searchtype=author&query=Aune%2C+T">T. Aune</a>, <a href="/search/astro-ph?searchtype=author&query=Beilicke%2C+M">M. Beilicke</a>, <a href="/search/astro-ph?searchtype=author&query=Benbow%2C+W">W. Benbow</a>, <a href="/search/astro-ph?searchtype=author&query=Boltuch%2C+D">D. Boltuch</a>, <a href="/search/astro-ph?searchtype=author&query=Bradbury%2C+S+M">S. M. Bradbury</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+J+H">J. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Bugaev%2C+V">V. Bugaev</a>, <a href="/search/astro-ph?searchtype=author&query=Byrum%2C+K">K. Byrum</a>, <a href="/search/astro-ph?searchtype=author&query=Cannon%2C+A">A. Cannon</a>, <a href="/search/astro-ph?searchtype=author&query=Cesarini%2C+A">A. Cesarini</a>, <a href="/search/astro-ph?searchtype=author&query=Ciupik%2C+L">L. Ciupik</a>, <a href="/search/astro-ph?searchtype=author&query=Cui%2C+W">W. Cui</a>, <a href="/search/astro-ph?searchtype=author&query=Dickherber%2C+R">R. Dickherber</a>, <a href="/search/astro-ph?searchtype=author&query=Duke%2C+C">C. Duke</a>, <a href="/search/astro-ph?searchtype=author&query=Falcone%2C+A">A. Falcone</a>, <a href="/search/astro-ph?searchtype=author&query=Finley%2C+J+P">J. P. Finley</a>, <a href="/search/astro-ph?searchtype=author&query=Finnegan%2C+G">G. Finnegan</a>, <a href="/search/astro-ph?searchtype=author&query=Fortson%2C+L">L. Fortson</a>, <a href="/search/astro-ph?searchtype=author&query=Furniss%2C+A">A. Furniss</a>, <a href="/search/astro-ph?searchtype=author&query=Galante%2C+N">N. Galante</a>, <a href="/search/astro-ph?searchtype=author&query=Gall%2C+D">D. Gall</a>, <a href="/search/astro-ph?searchtype=author&query=Gillanders%2C+G+H">G. H. Gillanders</a> , et al. (81 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="1106.1210v2-abstract-short" style="display: inline;"> We report on TeV gamma-ray observations of the blazar Mrk 421 (redshift of 0.031) with the VERITAS observatory and the Whipple 10m Cherenkov telescope. The excellent sensitivity of VERITAS allowed us to sample the TeV gamma-ray fluxes and energy spectra with unprecedented accuracy where Mrk 421 was detected in each of the pointings. A total of 47.3 hrs of VERITAS and 96 hrs of Whipple 10m data wer… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1106.1210v2-abstract-full').style.display = 'inline'; document.getElementById('1106.1210v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1106.1210v2-abstract-full" style="display: none;"> We report on TeV gamma-ray observations of the blazar Mrk 421 (redshift of 0.031) with the VERITAS observatory and the Whipple 10m Cherenkov telescope. The excellent sensitivity of VERITAS allowed us to sample the TeV gamma-ray fluxes and energy spectra with unprecedented accuracy where Mrk 421 was detected in each of the pointings. A total of 47.3 hrs of VERITAS and 96 hrs of Whipple 10m data were acquired between January 2006 and June 2008. We present the results of a study of the TeV gamma-ray energy spectra as a function of time, and for different flux levels. On May 2nd and 3rd, 2008, bright TeV gamma-ray flares were detected with fluxes reaching the level of 10 Crab. The TeV gamma-ray data were complemented with radio, optical, and X-ray observations, with flux variability found in all bands except for the radio waveband. The combination of the RXTE and Swift X-ray data reveal spectral hardening with increasing flux levels, often correlated with an increase of the source activity in TeV gamma-rays. Contemporaneous spectral energy distributions were generated for 18 nights, each of which are reasonably described by a one-zone SSC model. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1106.1210v2-abstract-full').style.display = 'none'; document.getElementById('1106.1210v2-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 June, 2011; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 June, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">30 pages, 12 figures, accepted by ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ, 738, 25 (2011) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1104.5094">arXiv:1104.5094</a> <span> [<a href="https://arxiv.org/pdf/1104.5094">pdf</a>, <a href="https://arxiv.org/ps/1104.5094">ps</a>, <a href="https://arxiv.org/format/1104.5094">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/735/2/85">10.1088/0004-637X/735/2/85 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> OGLE-2005-BLG-018: Characterization of Full Physical and Orbital Parameters of a Gravitational Binary Lens </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I+-">I. -G. Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">A. Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">C. Han</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">A. Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Dominik%2C+M">M. Dominik</a>, <a href="/search/astro-ph?searchtype=author&query=Fouque%2C+P">P. Fouque</a>, <a href="/search/astro-ph?searchtype=author&query=Kubiak%2C+M">M. Kubiak</a>, <a href="/search/astro-ph?searchtype=author&query=Szymanski%2C+M+K">M. K. Szymanski</a>, <a href="/search/astro-ph?searchtype=author&query=Pietrzynki%2C+G">G. Pietrzynki</a>, <a href="/search/astro-ph?searchtype=author&query=Soszynski%2C+I">I. Soszynski</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">K. Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Wyrzykowski%2C+L">L. Wyrzykowski</a>, <a href="/search/astro-ph?searchtype=author&query=DePoy%2C+D+L">D. L. DePoy</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+S">S. Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Gaudi%2C+B+S">B. S. Gaudi</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C+-">C. -U. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B+-">B. -G. Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">R. W. Pogge</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">M. D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Allan%2C+A">A. Allan</a>, <a href="/search/astro-ph?searchtype=author&query=Beaulieu%2C+J+P">J. P. Beaulieu</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+D+P">D. P. Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Bode%2C+M">M. Bode</a>, <a href="/search/astro-ph?searchtype=author&query=Bramich%2C+D+M">D. M. Bramich</a>, <a href="/search/astro-ph?searchtype=author&query=Brillant%2C+S">S. Brillant</a> , et al. (33 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="1104.5094v1-abstract-short" style="display: inline;"> We present the analysis result of a gravitational binary-lensing event OGLE-2005-BLG-018. The light curve of the event is characterized by 2 adjacent strong features and a single weak feature separated from the strong features. The light curve exhibits noticeable deviations from the best-fit model based on standard binary parameters. To explain the deviation, we test models including various highe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1104.5094v1-abstract-full').style.display = 'inline'; document.getElementById('1104.5094v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1104.5094v1-abstract-full" style="display: none;"> We present the analysis result of a gravitational binary-lensing event OGLE-2005-BLG-018. The light curve of the event is characterized by 2 adjacent strong features and a single weak feature separated from the strong features. The light curve exhibits noticeable deviations from the best-fit model based on standard binary parameters. To explain the deviation, we test models including various higher-order effects of the motions of the observer, source, and lens. From this, we find that it is necessary to account for the orbital motion of the lens in describing the light curve. From modeling of the light curve considering the parallax effect and Keplerian orbital motion, we are able to measure not only the physical parameters but also a complete orbital solution of the lens system. It is found that the event was produced by a binary lens located in the Galactic bulge with a distance $6.7\pm 0.3$ kpc from the Earth. The individual lens components with masses $0.9\pm 0.3\ M_\odot$ and $0.5\pm 0.1\ M_\odot$ are separated with a semi-major axis of $a=2.5 \pm 1.0$ AU and orbiting each other with a period $P=3.1 \pm 1.3$ yr. The event demonstrates that it is possible to extract detailed information about binary lens systems from well-resolved lensing light curves. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1104.5094v1-abstract-full').style.display = 'none'; document.getElementById('1104.5094v1-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 April, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">19 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/1101.3312">arXiv:1101.3312</a> <span> [<a href="https://arxiv.org/pdf/1101.3312">pdf</a>, <a href="https://arxiv.org/ps/1101.3312">ps</a>, <a href="https://arxiv.org/format/1101.3312">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/738/1/87">10.1088/0004-637X/738/1/87 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Binary microlensing event OGLE-2009-BLG-020 gives a verifiable mass, distance and orbit predictions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+J">J. Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">A. Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">A. Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+S">Subo Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Monard%2C+L+A+G">L. A. G. Monard</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">C. Han</a>, <a href="/search/astro-ph?searchtype=author&query=Nelson%2C+C+R">C. R. Nelson</a>, <a href="/search/astro-ph?searchtype=author&query=McCormick%2C+J">J. McCormick</a>, <a href="/search/astro-ph?searchtype=author&query=Moorhouse%2C+D">D. Moorhouse</a>, <a href="/search/astro-ph?searchtype=author&query=Thornley%2C+G">G. Thornley</a>, <a href="/search/astro-ph?searchtype=author&query=Maury%2C+A">A. Maury</a>, <a href="/search/astro-ph?searchtype=author&query=Bramich%2C+D+M">D. M. Bramich</a>, <a href="/search/astro-ph?searchtype=author&query=Greenhill%2C+J">J. Greenhill</a>, <a href="/search/astro-ph?searchtype=author&query=Kozlowski%2C+S">S. Kozlowski</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+I">I. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Poleski%2C+R">R. Poleski</a>, <a href="/search/astro-ph?searchtype=author&query=Wyrzykowski%2C+L">L. Wyrzykowski</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">K. Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Kubiak%2C+M">M. Kubiak</a>, <a href="/search/astro-ph?searchtype=author&query=Szymanski%2C+M+K">M. K. Szymanski</a>, <a href="/search/astro-ph?searchtype=author&query=Pietrzynski%2C+G">G. Pietrzynski</a>, <a href="/search/astro-ph?searchtype=author&query=Soszynski%2C+I">I. Soszynski</a>, <a href="/search/astro-ph?searchtype=author&query=Gaudi%2C+B+S">B. S. Gaudi</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">J. C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Hung%2C+L+-">L. -W. Hung</a> , et al. (77 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="1101.3312v1-abstract-short" style="display: inline;"> We present the first example of binary microlensing for which the parameter measurements can be verified (or contradicted) by future Doppler observations. This test is made possible by a confluence of two relatively unusual circumstances. First, the binary lens is bright enough (I=15.6) to permit Doppler measurements. Second, we measure not only the usual 7 binary-lens parameters, but also the 'mi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1101.3312v1-abstract-full').style.display = 'inline'; document.getElementById('1101.3312v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1101.3312v1-abstract-full" style="display: none;"> We present the first example of binary microlensing for which the parameter measurements can be verified (or contradicted) by future Doppler observations. This test is made possible by a confluence of two relatively unusual circumstances. First, the binary lens is bright enough (I=15.6) to permit Doppler measurements. Second, we measure not only the usual 7 binary-lens parameters, but also the 'microlens parallax' (which yields the binary mass) and two components of the instantaneous orbital velocity. Thus we measure, effectively, 6 'Kepler+1' parameters (two instantaneous positions, two instantaneous velocities, the binary total mass, and the mass ratio). Since Doppler observations of the brighter binary component determine 5 Kepler parameters (period, velocity amplitude, eccentricity, phase, and position of periapsis), while the same spectroscopy yields the mass of the primary, the combined Doppler + microlensing observations would be overconstrained by 6 + (5 + 1) - (7 + 1) = 4 degrees of freedom. This makes possible an extremely strong test of the microlensing solution. We also introduce a uniform microlensing notation for single and binary lenses, we define conventions, summarize all known microlensing degeneracies and extend a set of parameters to describe full Keplerian motion of the binary lenses. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1101.3312v1-abstract-full').style.display = 'none'; document.getElementById('1101.3312v1-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 January, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">51 pages, 8 figures, 2 appendices. Submitted to ApJ. Fortran codes for Appendix B are attached to this astro-ph submission and are also available at http://www.astronomy.ohio-state.edu/~jskowron/OGLE-2009-BLG-020/</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1012.4486">arXiv:1012.4486</a> <span> [<a href="https://arxiv.org/pdf/1012.4486">pdf</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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <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"> Completing the Census of Exoplanets with the Microlensing Planet Finder (MPF) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+D+P">David P. Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Beaulieu%2C+J+-">J. -P. Beaulieu</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+I">I. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+E">E. Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K">K. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Friedman%2C+S">S. Friedman</a>, <a href="/search/astro-ph?searchtype=author&query=Gaudi%2C+B+S">B. S. Gaudi</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">A. Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Jenkins%2C+J">J. Jenkins</a>, <a href="/search/astro-ph?searchtype=author&query=Kimble%2C+R">R. Kimble</a>, <a href="/search/astro-ph?searchtype=author&query=Lin%2C+D">D. Lin</a>, <a href="/search/astro-ph?searchtype=author&query=Mather%2C+J">J. Mather</a>, <a href="/search/astro-ph?searchtype=author&query=Rich%2C+M">M. Rich</a>, <a href="/search/astro-ph?searchtype=author&query=Sahu%2C+K">K. Sahu</a>, <a href="/search/astro-ph?searchtype=author&query=Shao%2C+M">M. Shao</a>, <a href="/search/astro-ph?searchtype=author&query=Sumi%2C+T">T. Sumi</a>, <a href="/search/astro-ph?searchtype=author&query=Tenerelli%2C+D">D. Tenerelli</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">A. Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Yock%2C+P">P. Yock</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="1012.4486v1-abstract-short" style="display: inline;"> The MPF mission will provide a statistical census of exoplanets with masses greater than 0.1 Earth-masses and orbital separations ranging from 0.5AU to infinity. This includes analogs to all the Solar System's planets except for Mercury, as well as most types of planets predicted by planet formation theories. Such a survey will provide results on the frequency of planets around all types of stars… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1012.4486v1-abstract-full').style.display = 'inline'; document.getElementById('1012.4486v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1012.4486v1-abstract-full" style="display: none;"> The MPF mission will provide a statistical census of exoplanets with masses greater than 0.1 Earth-masses and orbital separations ranging from 0.5AU to infinity. This includes analogs to all the Solar System's planets except for Mercury, as well as most types of planets predicted by planet formation theories. Such a survey will provide results on the frequency of planets around all types of stars except those with short lifetimes. Close-in planets with separations < 0.5 AU are invisible to a space-based microlensing survey, but these can be found by Kepler. Other methods, including ground-based microlensing, cannot approach the comprehensive statistics on the mass and semi-major axis distribution of extrasolar planets that a space-based microlensing survey will provide. The terrestrial planet sensitivity of a ground-based microlensing survey is limited to the vicinity of the Einstein radius at 2-3 AU, and space-based imaging is needed to identify and determine the mass of the planetary host stars for the vast majority of planets discovered by microlensing. Thus, a space-based microlensing survey is likely to be the only way to gain a comprehensive understanding of the architecture of planetary systems, which is needed to understand planet formation and habitability. MPF can accomplish these objectives with proven technology and a cost of $333 million (excluding launch vehicle). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1012.4486v1-abstract-full').style.display = 'none'; document.getElementById('1012.4486v1-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 December, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2010. </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">RFI Response for the Astro2010 Program Prioritization Panel, (The Basis for the Exoplanet Program of the WFIRST Mission)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1009.0344">arXiv:1009.0344</a> <span> [<a href="https://arxiv.org/pdf/1009.0344">pdf</a>, <a href="https://arxiv.org/ps/1009.0344">ps</a>, <a href="https://arxiv.org/format/1009.0344">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/723/1/797">10.1088/0004-637X/723/1/797 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> OGLE-2005-BLG-153: Microlensing Discovery and Characterization of A Very Low Mass Binary </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K+-">K. -H. Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">A. Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">C. Han</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y+-">Y. -H. Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+I+A">I. A. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Beaulieu%2C+J+-">J. -P. Beaulieu</a>, <a href="/search/astro-ph?searchtype=author&query=Dominik%2C+M">M. Dominik</a>, <a href="/search/astro-ph?searchtype=author&query=Horne%2C+K">K. Horne</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">A. Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Gaudi%2C+B+S">B. S. Gaudi</a>, <a href="/search/astro-ph?searchtype=author&query=Kubiak%2C+M">M. Kubiak</a>, <a href="/search/astro-ph?searchtype=author&query=Szymanski%2C+M+K">M. K. Szymanski</a>, <a href="/search/astro-ph?searchtype=author&query=Pietrzynski%2C+G">G. Pietrzynski</a>, <a href="/search/astro-ph?searchtype=author&query=Soszynski%2C+I">I. Soszynski</a>, <a href="/search/astro-ph?searchtype=author&query=Szewczyk%2C+O">O. Szewczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">K. Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Wyrzykowski%2C+L">L. Wyrzykowski</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+F">F. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Botzler%2C+C+S">C. S. Botzler</a>, <a href="/search/astro-ph?searchtype=author&query=Hearnshaw%2C+J+B">J. B. Hearnshaw</a>, <a href="/search/astro-ph?searchtype=author&query=Itow%2C+Y">Y. Itow</a>, <a href="/search/astro-ph?searchtype=author&query=Kamiya%2C+K">K. Kamiya</a>, <a href="/search/astro-ph?searchtype=author&query=Kilmartin%2C+P+M">P. M. Kilmartin</a>, <a href="/search/astro-ph?searchtype=author&query=Masuda%2C+K">K. Masuda</a>, <a href="/search/astro-ph?searchtype=author&query=Matsubara%2C+Y">Y. Matsubara</a> , et al. (55 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="1009.0344v2-abstract-short" style="display: inline;"> The mass function and statistics of binaries provide important diagnostics of the star formation process. Despite this importance, the mass function at low masses remains poorly known due to observational difficulties caused by the faintness of the objects. Here we report the microlensing discovery and characterization of a binary lens composed of very low-mass stars just above the hydrogen-burnin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1009.0344v2-abstract-full').style.display = 'inline'; document.getElementById('1009.0344v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1009.0344v2-abstract-full" style="display: none;"> The mass function and statistics of binaries provide important diagnostics of the star formation process. Despite this importance, the mass function at low masses remains poorly known due to observational difficulties caused by the faintness of the objects. Here we report the microlensing discovery and characterization of a binary lens composed of very low-mass stars just above the hydrogen-burning limit. From the combined measurements of the Einstein radius and microlens parallax, we measure the masses of the binary components of $0.10\pm 0.01\ M_\odot$ and $0.09\pm 0.01\ M_\odot$. This discovery demonstrates that microlensing will provide a method to measure the mass function of all Galactic populations of very low mass binaries that is independent of the biases caused by the luminosity of the population. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1009.0344v2-abstract-full').style.display = 'none'; document.getElementById('1009.0344v2-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 April, 2012; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 September, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2010. </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, 3 figures, 1 table</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1008.3727">arXiv:1008.3727</a> <span> [<a href="https://arxiv.org/pdf/1008.3727">pdf</a>, <a href="https://arxiv.org/ps/1008.3727">ps</a>, <a href="https://arxiv.org/format/1008.3727">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-6256/140/6/1719">10.1088/0004-6256/140/6/1719 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First Results from the NOAO Survey of the Outer Limits of the Magellanic Clouds </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Saha%2C+A">Abhijit Saha</a>, <a href="/search/astro-ph?searchtype=author&query=Olszewski%2C+E+W">Edward W. Olszewski</a>, <a href="/search/astro-ph?searchtype=author&query=Brondel%2C+B">Brian Brondel</a>, <a href="/search/astro-ph?searchtype=author&query=Olsen%2C+K">Knut Olsen</a>, <a href="/search/astro-ph?searchtype=author&query=Knezek%2C+P">Patricia Knezek</a>, <a href="/search/astro-ph?searchtype=author&query=Harris%2C+J">Jason Harris</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+C">Chris Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Subramaniam%2C+A">Annapurni Subramaniam</a>, <a href="/search/astro-ph?searchtype=author&query=Claver%2C+J">Jennifer Claver</a>, <a href="/search/astro-ph?searchtype=author&query=Rest%2C+A">Armin Rest</a>, <a href="/search/astro-ph?searchtype=author&query=Seitzer%2C+P">Patrick Seitzer</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K+H">Kem H. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">Dante Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Suntzeff%2C+N+B">Nicholas B. Suntzeff</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="1008.3727v1-abstract-short" style="display: inline;"> [abridged] We describe the first results from the NOAO Outer Limits Survey. The survey consists of deep images of 55 0.6x0.6 degree fields at distances up to 20 degrees from the LMC/SMC, and 10 controls. The fields probe the outer structure of the Clouds, the Magellanic Stream, the Leading Arm, and the wake of the new LMC orbit. Images were taken in 5 filters on the CTIO Blanco 4-m and Mosaic2 cam… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1008.3727v1-abstract-full').style.display = 'inline'; document.getElementById('1008.3727v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1008.3727v1-abstract-full" style="display: none;"> [abridged] We describe the first results from the NOAO Outer Limits Survey. The survey consists of deep images of 55 0.6x0.6 degree fields at distances up to 20 degrees from the LMC/SMC, and 10 controls. The fields probe the outer structure of the Clouds, the Magellanic Stream, the Leading Arm, and the wake of the new LMC orbit. Images were taken in 5 filters on the CTIO Blanco 4-m and Mosaic2 camera, with calibration at the CTIO 0.9-m. The CRI images reach depths below the oldest LMC/SMC main sequence (MS) turnoffs, yielding probes of structure combined with ability to measure stellar ages and metallicities. M and DDO51 images allow for discrimination of LMC and SMC giant stars from foreground dwarfs, allowing us to use giants as additional probes. From photometry of 8 fields at radii of 7-19 degrees N of the LMC bar, we find MS stars associated with the LMC to 16 degrees from the LMC center, while the much rarer giants can only be convincingly detected out to 11 degrees. In one control field, we see the signature of the Milky Way globular cluster NGC 1851. The CMDs show that while at 7-degree radius LMC populations as young as 500 Myr are present, at radii more than 11 degrees only the underlying old metal-poor population remains, demonstrating the existence of a population gradient. Even at extreme distances, the dominant age is much less than "globular Cluster age." MS star counts follow an exponential decline with a scale length of 1.15 kpc, essentially the same scale length as gleaned for the inner LMC disk from prior studies. While we cannot rule out tidal structure elsewhere, detection of ordered structure to 12 disk scale lengths is unprecedented, and adds to the puzzle of the LMC's interaction history. Our results do not rule out the possible existence of an LMC stellar halo, which may only dominate the disk at yet larger radii. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1008.3727v1-abstract-full').style.display = 'none'; document.getElementById('1008.3727v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 August, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2010. </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 AJ; full-resolution postscript of entire article can be found at http://adansonia.as.arizona.edu/~edo/astro-ph/ms.ps</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1007.5029">arXiv:1007.5029</a> <span> [<a href="https://arxiv.org/pdf/1007.5029">pdf</a>, <a href="https://arxiv.org/format/1007.5029">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/723/2/1195">10.1088/0004-637X/723/2/1195 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Infrared Period-Luminosity Relations of Evolved Variable Stars in the Large Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Riebel%2C+D">David Riebel</a>, <a href="/search/astro-ph?searchtype=author&query=Meixner%2C+M">Margaret Meixner</a>, <a href="/search/astro-ph?searchtype=author&query=Fraser%2C+O">Oliver Fraser</a>, <a href="/search/astro-ph?searchtype=author&query=Srinivasan%2C+S">Sundar Srinivasan</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K">Kem Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Vijh%2C+U">Uma Vijh</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="1007.5029v1-abstract-short" style="display: inline;"> We combine variability information from the MAssive Compact Halo Objects (MACHO) survey of the Large Magellanic Cloud (LMC) with infrared photometry from the Spitzer Space Telescope Surveying the Agents of a Galaxy's Evolution (SAGE) survey to create a dataset of ~30 000 variable red sources. We photometrically classify these sources as being on the first ascent of the Red Giant Branch (RGB), or a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1007.5029v1-abstract-full').style.display = 'inline'; document.getElementById('1007.5029v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1007.5029v1-abstract-full" style="display: none;"> We combine variability information from the MAssive Compact Halo Objects (MACHO) survey of the Large Magellanic Cloud (LMC) with infrared photometry from the Spitzer Space Telescope Surveying the Agents of a Galaxy's Evolution (SAGE) survey to create a dataset of ~30 000 variable red sources. We photometrically classify these sources as being on the first ascent of the Red Giant Branch (RGB), or as being in one of three stages along the Asymptotic Giant Branch (AGB): oxygen-rich, carbon-rich, or highly reddened with indeterminate chemistry ("extreme" AGB candidates). We present linear period-luminosity relationships for these sources using 8 separate infrared bands (J, H, K, 3.6, 4.5, 5.8, 8.0, and 24 micron) as proxies for the luminosity. We find that the wavelength dependence of the slope of the period-luminosity relationship is different for different photometrically determined classes of AGB stars. Stars photometrically classified as O-rich show the least variation of slope with wavelength, while dust enshrouded extreme AGB stars show a pronounced trend toward steeper slopes with increasing wavelength. We find that O-rich AGB stars pulsating in the fundamental mode obey a period-magnitude relation with a slope of -3.41 +/- 0.04 when magnitude is measured in the 3.6 micron band, in contrast to C-rich AGB stars, which obey a relation of slope -3.77 +/- 0.05. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1007.5029v1-abstract-full').style.display = 'none'; document.getElementById('1007.5029v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 July, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2010. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1005.0966">arXiv:1005.0966</a> <span> [<a href="https://arxiv.org/pdf/1005.0966">pdf</a>, <a href="https://arxiv.org/ps/1005.0966">ps</a>, <a href="https://arxiv.org/format/1005.0966">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/10.1051/0004-6361/201014053">10.1051/0004-6361/201014053 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> OGLE 2008--BLG--290: An accurate measurement of the limb darkening of a Galactic Bulge K Giant spatially resolved by microlensing </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Fouque%2C+P">P. Fouque</a>, <a href="/search/astro-ph?searchtype=author&query=Heyrovsky%2C+D">D. Heyrovsky</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+S">S. Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">A. Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">A. Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">M. D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+V">V. Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Beaulieu%2C+J+-">J. -P. Beaulieu</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+D+P">D. P. Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+I+A">I. A. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Bramich%2C+D+M">D. M. Bramich</a>, <a href="/search/astro-ph?searchtype=author&query=Novati%2C+S+C">S. Calchi Novati</a>, <a href="/search/astro-ph?searchtype=author&query=Cassan%2C+A">A. Cassan</a>, <a href="/search/astro-ph?searchtype=author&query=Coutures%2C+C">C. Coutures</a>, <a href="/search/astro-ph?searchtype=author&query=Dieters%2C+S">S. Dieters</a>, <a href="/search/astro-ph?searchtype=author&query=Dominik%2C+M">M. Dominik</a>, <a href="/search/astro-ph?searchtype=author&query=Prester%2C+D+D">D. Dominis Prester</a>, <a href="/search/astro-ph?searchtype=author&query=Greenhill%2C+J">J. Greenhill</a>, <a href="/search/astro-ph?searchtype=author&query=Horne%2C+K">K. Horne</a>, <a href="/search/astro-ph?searchtype=author&query=Jorgensen%2C+U+G">U. G. Jorgensen</a>, <a href="/search/astro-ph?searchtype=author&query=Kozlowski%2C+S">S. Kozlowski</a>, <a href="/search/astro-ph?searchtype=author&query=Kubas%2C+D">D. Kubas</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C+-">C. -H. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Marquette%2C+J+-">J. -B. Marquette</a>, <a href="/search/astro-ph?searchtype=author&query=Mathiasen%2C+M">M. Mathiasen</a> , et al. (93 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="1005.0966v1-abstract-short" style="display: inline;"> Gravitational microlensing is not only a successful tool for discovering distant exoplanets, but it also enables characterization of the lens and source stars involved in the lensing event. In high magnification events, the lens caustic may cross over the source disk, which allows a determination of the angular size of the source and additionally a measurement of its limb darkening. When such exte… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1005.0966v1-abstract-full').style.display = 'inline'; document.getElementById('1005.0966v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1005.0966v1-abstract-full" style="display: none;"> Gravitational microlensing is not only a successful tool for discovering distant exoplanets, but it also enables characterization of the lens and source stars involved in the lensing event. In high magnification events, the lens caustic may cross over the source disk, which allows a determination of the angular size of the source and additionally a measurement of its limb darkening. When such extended-source effects appear close to maximum magnification, the resulting light curve differs from the characteristic Paczynski point-source curve. The exact shape of the light curve close to the peak depends on the limb darkening of the source. Dense photometric coverage permits measurement of the respective limb-darkening coefficients. In the case of microlensing event OGLE 2008-BLG-290, the K giant source star reached a peak magnification of about 100. Thirteen different telescopes have covered this event in eight different photometric bands. Subsequent light-curve analysis yielded measurements of linear limb-darkening coefficients of the source in six photometric bands. The best-measured coefficients lead to an estimate of the source effective temperature of about 4700 +100-200 K. However, the photometric estimate from colour-magnitude diagrams favours a cooler temperature of 4200 +-100 K. As the limb-darkening measurements, at least in the CTIO/SMARTS2 V and I bands, are among the most accurate obtained, the above disagreement needs to be understood. A solution is proposed, which may apply to previous events where such a discrepancy also appeared. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1005.0966v1-abstract-full').style.display = 'none'; document.getElementById('1005.0966v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 May, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2010. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Astronomy & Astrophysics in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1004.0955">arXiv:1004.0955</a> <span> [<a href="https://arxiv.org/pdf/1004.0955">pdf</a>, <a href="https://arxiv.org/ps/1004.0955">ps</a>, <a href="https://arxiv.org/format/1004.0955">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="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-6256/140/2/328">10.1088/0004-6256/140/2/328 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> High Amplitude 未-Scutis in the Large Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Garg%2C+A">A. Garg</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K+H">K. H. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Nikolaev%2C+S">S. Nikolaev</a>, <a href="/search/astro-ph?searchtype=author&query=Huber%2C+M+E">M. E. Huber</a>, <a href="/search/astro-ph?searchtype=author&query=Rest%2C+A">A. Rest</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+A+C">A. C. Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Challis%2C+P">P. Challis</a>, <a href="/search/astro-ph?searchtype=author&query=Clocchiatti%2C+A">A. Clocchiatti</a>, <a href="/search/astro-ph?searchtype=author&query=Miknaitis%2C+G">G. Miknaitis</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Morelli%2C+L">L. Morelli</a>, <a href="/search/astro-ph?searchtype=author&query=Olsen%2C+K">K. Olsen</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+J+L">J. L. Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Suntzeff%2C+N+B">N. B. Suntzeff</a>, <a href="/search/astro-ph?searchtype=author&query=Welch%2C+D+L">D. L. Welch</a>, <a href="/search/astro-ph?searchtype=author&query=Wood-Vasey%2C+W+M">W. M. Wood-Vasey</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="1004.0955v1-abstract-short" style="display: inline;"> We present 2323 High-Amplitude 未-Scuti (HADS) candidates discovered in the Large Magellanic Cloud (LMC) by the SuperMACHO survey (Rest et al. 2005). Frequency analyses of these candidates reveal that several are multimode pulsators, including 119 whose largest amplitude of pulsation is in the fundamental (F) mode and 19 whose largest amplitude of pulsation is in the first overtone (FO) mode. Usi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1004.0955v1-abstract-full').style.display = 'inline'; document.getElementById('1004.0955v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1004.0955v1-abstract-full" style="display: none;"> We present 2323 High-Amplitude 未-Scuti (HADS) candidates discovered in the Large Magellanic Cloud (LMC) by the SuperMACHO survey (Rest et al. 2005). Frequency analyses of these candidates reveal that several are multimode pulsators, including 119 whose largest amplitude of pulsation is in the fundamental (F) mode and 19 whose largest amplitude of pulsation is in the first overtone (FO) mode. Using Fourier decomposition of the HADS light curves, we find that the period-luminosity (PL) relation defined by the FO pulsators does not show a clear separation from the PL-relation defined by the F pulsators. This differs from other instability strip pulsators such as type c RR Lyrae. We also present evidence for a larger amplitude, subluminous population of HADS similar to that observed in Fornax (Poretti et al. 2008). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1004.0955v1-abstract-full').style.display = 'none'; document.getElementById('1004.0955v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 April, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2010. </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, 15 figures, AJ accepted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1003.2526">arXiv:1003.2526</a> <span> [<a href="https://arxiv.org/pdf/1003.2526">pdf</a>, <a href="https://arxiv.org/ps/1003.2526">ps</a>, <a href="https://arxiv.org/format/1003.2526">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/10.1088/0004-6256/139/5/2026">10.1088/0004-6256/139/5/2026 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The TAOS Project Stellar Variability II. Detection of 15 Variable Stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mondal%2C+S">S. Mondal</a>, <a href="/search/astro-ph?searchtype=author&query=Lin%2C+C+C">C. C. Lin</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W+P">W. P. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+Z+-">Z. -W. Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Alcock%2C+C">C. Alcock</a>, <a href="/search/astro-ph?searchtype=author&query=Axelrod%2C+T">T. Axelrod</a>, <a href="/search/astro-ph?searchtype=author&query=Bianco%2C+F+B">F. B. Bianco</a>, <a href="/search/astro-ph?searchtype=author&query=Byun%2C+Y+-">Y. -I. Byun</a>, <a href="/search/astro-ph?searchtype=author&query=Coehlo%2C+N+K">N. K. Coehlo</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K+H">K. H. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Dave%2C+R">R. Dave</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D+-">D. -W. Kim</a>, <a href="/search/astro-ph?searchtype=author&query=King%2C+S+-">S. -K. King</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+T">T. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lehner%2C+M+J">M. J. Lehner</a>, <a href="/search/astro-ph?searchtype=author&query=Lin%2C+H+-">H. -C. Lin</a>, <a href="/search/astro-ph?searchtype=author&query=Marshal%2C+S+L">S. L. Marshal</a>, <a href="/search/astro-ph?searchtype=author&query=Protopapas%2C+P">P. Protopapas</a>, <a href="/search/astro-ph?searchtype=author&query=Rice%2C+J+A">J. A. Rice</a>, <a href="/search/astro-ph?searchtype=author&query=Schwamb%2C+M+E">M. E. Schwamb</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+J+-">J. -H. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+S+-">S. -Y. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Wen%2C+C+-">C. -Y. Wen</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1003.2526v1-abstract-short" style="display: inline;"> The Taiwanese-American Occultation Survey (TAOS) project has collected more than a billion photometric measurements since 2005 January. These sky survey data-covering timescales from a fraction of a second to a few hundred days-are a useful source to study stellar variability. A total of 167 star fields, mostly along the ecliptic plane, have been selected for photometric monitoring with the TAOS… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1003.2526v1-abstract-full').style.display = 'inline'; document.getElementById('1003.2526v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1003.2526v1-abstract-full" style="display: none;"> The Taiwanese-American Occultation Survey (TAOS) project has collected more than a billion photometric measurements since 2005 January. These sky survey data-covering timescales from a fraction of a second to a few hundred days-are a useful source to study stellar variability. A total of 167 star fields, mostly along the ecliptic plane, have been selected for photometric monitoring with the TAOS telescopes. This paper presents our initial analysis of a search for periodic variable stars from the time-series TAOS data on one particular TAOS field, No. 151 (RA = 17$^{\rm h}30^{\rm m}6\fs$67, Dec = 27\degr17\arcmin 30\arcsec, J2000), which had been observed over 47 epochs in 2005. A total of 81 candidate variables are identified in the 3 square degree field, with magnitudes in the range 8 < R < 16. On the basis of the periodicity and shape of the lightcurves, 29 variables, 15 of which were previously unknown, are classified as RR Lyrae, Cepheid, delta Scuti, SX Phonencis, semi-regular and eclipsing binaries. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1003.2526v1-abstract-full').style.display = 'none'; document.getElementById('1003.2526v1-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 March, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2010. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 6 figures, accepted 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/1002.3626">arXiv:1002.3626</a> <span> [<a href="https://arxiv.org/pdf/1002.3626">pdf</a>, <a href="https://arxiv.org/ps/1002.3626">ps</a>, <a href="https://arxiv.org/format/1002.3626">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/10.1086/655443">10.1086/655443 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The TAOS Project: Statistical Analysis of Multi-Telescope Time Series Data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lehner%2C+M+J">M. J. Lehner</a>, <a href="/search/astro-ph?searchtype=author&query=Coehlo%2C+N+K">N. K. Coehlo</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+Z+-">Z. -W. Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Bianco%2C+F+B">F. B. Bianco</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+J+-">J. -H. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Rice%2C+J+A">J. A. Rice</a>, <a href="/search/astro-ph?searchtype=author&query=Protopapas%2C+P">P. Protopapas</a>, <a href="/search/astro-ph?searchtype=author&query=Alcock%2C+C">C. Alcock</a>, <a href="/search/astro-ph?searchtype=author&query=Axelrod%2C+T">T. Axelrod</a>, <a href="/search/astro-ph?searchtype=author&query=Byun%2C+Y+-">Y. -I. Byun</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W+P">W. P. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K+H">K. H. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=de+Pater%2C+I">I. de Pater</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D+-">D. -W. Kim</a>, <a href="/search/astro-ph?searchtype=author&query=King%2C+S+-">S. -K. King</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+T">T. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+S+L">S. L. Marshall</a>, <a href="/search/astro-ph?searchtype=author&query=Schwamb%2C+M+E">M. E. Schwamb</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+S+-">S. -Y. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Wen%2C+C+-">C. -Y. Wen</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="1002.3626v1-abstract-short" style="display: inline;"> The Taiwanese-American Occultation Survey (TAOS) monitors fields of up to ~1000 stars at 5 Hz simultaneously with four small telescopes to detect occultation events from small (~1 km) Kuiper Belt Objects (KBOs). The survey presents a number of challenges, in particular the fact that the occultation events we are searching for are extremely rare and are typically manifested as slight flux drops f… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1002.3626v1-abstract-full').style.display = 'inline'; document.getElementById('1002.3626v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1002.3626v1-abstract-full" style="display: none;"> The Taiwanese-American Occultation Survey (TAOS) monitors fields of up to ~1000 stars at 5 Hz simultaneously with four small telescopes to detect occultation events from small (~1 km) Kuiper Belt Objects (KBOs). The survey presents a number of challenges, in particular the fact that the occultation events we are searching for are extremely rare and are typically manifested as slight flux drops for only one or two consecutive time series measurements. We have developed a statistical analysis technique to search the multi-telescope data set for simultaneous flux drops which provides a robust false positive rejection and calculation of event significance. In this paper, we describe in detail this statistical technique and its application to the TAOS data set. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1002.3626v1-abstract-full').style.display = 'none'; document.getElementById('1002.3626v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 February, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2010. </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, 14 figures. Submitted to PASP</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1001.2006">arXiv:1001.2006</a> <span> [<a href="https://arxiv.org/pdf/1001.2006">pdf</a>, <a href="https://arxiv.org/ps/1001.2006">ps</a>, <a href="https://arxiv.org/format/1001.2006">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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-6256/139/4/1499">10.1088/0004-6256/139/4/1499 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The TAOS Project: Upper Bounds on the Population of Small KBOs and Tests of Models of Formation and Evolution of the Outer Solar System </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bianco%2C+F+B">F. B. Bianco</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+Z+-">Z. -W. Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Lehner%2C+M+J">M. J. Lehner</a>, <a href="/search/astro-ph?searchtype=author&query=Mondal%2C+S">S. Mondal</a>, <a href="/search/astro-ph?searchtype=author&query=King%2C+S+-">S. -K. King</a>, <a href="/search/astro-ph?searchtype=author&query=Giammarco%2C+J">J. Giammarco</a>, <a href="/search/astro-ph?searchtype=author&query=Holman%2C+M+J">M. J. Holman</a>, <a href="/search/astro-ph?searchtype=author&query=Coehlo%2C+N+K">N. K. Coehlo</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+J+-">J. -H. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Alcock%2C+C">C. Alcock</a>, <a href="/search/astro-ph?searchtype=author&query=Axelrod%2C+T">T. Axelrod</a>, <a href="/search/astro-ph?searchtype=author&query=Byun%2C+Y+-">Y. -I. Byun</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W+P">W. P. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K+H">K. H. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Dave%2C+R">R. Dave</a>, <a href="/search/astro-ph?searchtype=author&query=de+Pater%2C+I">I. de Pater</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D+-">D. -W. Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+T">T. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lin%2C+H+-">H. -C. Lin</a>, <a href="/search/astro-ph?searchtype=author&query=Lissauer%2C+J+J">J. J. Lissauer</a>, <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+S+L">S. L. Marshall</a>, <a href="/search/astro-ph?searchtype=author&query=Protopapas%2C+P">P. Protopapas</a>, <a href="/search/astro-ph?searchtype=author&query=Rice%2C+J+A">J. A. Rice</a>, <a href="/search/astro-ph?searchtype=author&query=Schwamb%2C+M+E">M. E. Schwamb</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+S+-">S. -Y. Wang</a> , et al. (1 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1001.2006v2-abstract-short" style="display: inline;"> We have analyzed the first 3.75 years of data from TAOS, the Taiwanese American Occultation Survey. TAOS monitors bright stars to search for occultations by Kuiper Belt Objects (KBOs). This dataset comprises 5e5 star-hours of multi-telescope photometric data taken at 4 or 5 Hz. No events consistent with KBO occultations were found in this dataset. We compute the number of events expected for the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1001.2006v2-abstract-full').style.display = 'inline'; document.getElementById('1001.2006v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1001.2006v2-abstract-full" style="display: none;"> We have analyzed the first 3.75 years of data from TAOS, the Taiwanese American Occultation Survey. TAOS monitors bright stars to search for occultations by Kuiper Belt Objects (KBOs). This dataset comprises 5e5 star-hours of multi-telescope photometric data taken at 4 or 5 Hz. No events consistent with KBO occultations were found in this dataset. We compute the number of events expected for the Kuiper Belt formation and evolution models of Pan & Sari (2005), Kenyon & Bromley (2004), Benavidez & Campo Bagatin (2009), and Fraser (2009). A comparison with the upper limits we derive from our data constrains the parameter space of these models. This is the first detailed comparison of models of the KBO size distribution with data from an occultation survey. Our results suggest that the KBO population is comprised of objects with low internal strength and that planetary migration played a role in the shaping of the size distribution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1001.2006v2-abstract-full').style.display = 'none'; document.getElementById('1001.2006v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 January, 2010; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 January, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2010. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 16 figures, Aj submitted</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2010 The Astronomical Journal 139 1499 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0912.2312">arXiv:0912.2312</a> <span> [<a href="https://arxiv.org/pdf/0912.2312">pdf</a>, <a href="https://arxiv.org/format/0912.2312">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/10.1051/0004-6361/200912007">10.1051/0004-6361/200912007 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Limb-darkening measurements for a cool red giant in microlensing event OGLE 2004-BLG-482 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zub%2C+M">M. Zub</a>, <a href="/search/astro-ph?searchtype=author&query=Cassan%2C+A">A. Cassan</a>, <a href="/search/astro-ph?searchtype=author&query=Heyrovsky%2C+D">D. Heyrovsky</a>, <a href="/search/astro-ph?searchtype=author&query=Fouque%2C+P">P. Fouque</a>, <a href="/search/astro-ph?searchtype=author&query=Stempels%2C+H+C">H. C. Stempels</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">M. D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Beaulieu%2C+J+-">J. -P. Beaulieu</a>, <a href="/search/astro-ph?searchtype=author&query=Brillant%2C+S">S. Brillant</a>, <a href="/search/astro-ph?searchtype=author&query=Christie%2C+G+W">G. W. Christie</a>, <a href="/search/astro-ph?searchtype=author&query=Kains%2C+N">N. Kains</a>, <a href="/search/astro-ph?searchtype=author&query=Kozlowski%2C+S">S. Kozlowski</a>, <a href="/search/astro-ph?searchtype=author&query=Kubas%2C+D">D. Kubas</a>, <a href="/search/astro-ph?searchtype=author&query=Wambsganss%2C+J">J. Wambsganss</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+V">V. Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+D+P">D. P. Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K">K. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Coutures%2C+C">C. Coutures</a>, <a href="/search/astro-ph?searchtype=author&query=Dieters%2C+S">S. Dieters</a>, <a href="/search/astro-ph?searchtype=author&query=Dominik%2C+M">M. Dominik</a>, <a href="/search/astro-ph?searchtype=author&query=Prester%2C+D+D">D. Dominis Prester</a>, <a href="/search/astro-ph?searchtype=author&query=Donatowicz%2C+J">J. Donatowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Greenhill%2C+J">J. Greenhill</a>, <a href="/search/astro-ph?searchtype=author&query=Horne%2C+K">K. Horne</a>, <a href="/search/astro-ph?searchtype=author&query=Jorgensen%2C+U+G">U. G. Jorgensen</a>, <a href="/search/astro-ph?searchtype=author&query=Kane%2C+S+R">S. R. Kane</a> , et al. (25 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0912.2312v2-abstract-short" style="display: inline;"> Aims: We present a detailed analysis of OGLE 2004-BLG-482, a relatively high-magnification single-lens microlensing event which exhibits clear extended-source effects. These events are relatively rare, but they potentially contain unique information on the stellar atmosphere properties of their source star, as shown in this study. Methods: Our dense photometric coverage of the overall light curve… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0912.2312v2-abstract-full').style.display = 'inline'; document.getElementById('0912.2312v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0912.2312v2-abstract-full" style="display: none;"> Aims: We present a detailed analysis of OGLE 2004-BLG-482, a relatively high-magnification single-lens microlensing event which exhibits clear extended-source effects. These events are relatively rare, but they potentially contain unique information on the stellar atmosphere properties of their source star, as shown in this study. Methods: Our dense photometric coverage of the overall light curve and a proper microlensing modelling allow us to derive measurements of the OGLE 2004-BLG-482 source star's linear limb-darkening coefficients in three bands, including standard Johnson-Cousins I and R, as well as in a broad clear filter. In particular, we discuss in detail the problems of multi-band and multi-site modelling on the expected precision of our results. We also obtained high-resolution UVES spectra as part of a ToO programme at ESO VLT from which we derive the source star's precise fundamental parameters. Results: From the high-resolution UVES spectra, we find that OGLE 2004-BLG-482's source star is a red giant of MK type a bit later than M3, with Teff = 3667 +/- 150 K, log g = 2.1 +/- 1.0 and an assumed solar metallicity. This is confirmed by an OGLE calibrated colour-magnitude diagram. We then obtain from a detailed microlensing modelling of the light curve linear limb-darkening coefficients that we compare to model-atmosphere predictions available in the literature, and find a very good agreement for the I and R bands. In addition, we perform a similar analysis using an alternative description of limb darkening based on a principal component analysis of ATLAS limb-darkening profiles, and also find a very good agreement between measurements and model predictions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0912.2312v2-abstract-full').style.display = 'none'; document.getElementById('0912.2312v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 September, 2010; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 December, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2009. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0912.1791">arXiv:0912.1791</a> <span> [<a href="https://arxiv.org/pdf/0912.1791">pdf</a>, <a href="https://arxiv.org/format/0912.1791">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-6256/139/2/757">10.1088/0004-6256/139/2/757 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The TAOS Project Stellar Variability I. Detection of Low-Amplitude delta Scuti Stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D+-">D. -W. Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Protopapas%2C+P">P. Protopapas</a>, <a href="/search/astro-ph?searchtype=author&query=Alcock%2C+C">C. Alcock</a>, <a href="/search/astro-ph?searchtype=author&query=Byun%2C+Y+-">Y. -I. Byun</a>, <a href="/search/astro-ph?searchtype=author&query=Kyeong%2C+J">J. Kyeong</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+B+-">B. -C. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Wright%2C+N+J">N. J. Wright</a>, <a href="/search/astro-ph?searchtype=author&query=Axelrod%2C+T">T. Axelrod</a>, <a href="/search/astro-ph?searchtype=author&query=Bianco%2C+F+B">F. B. Bianco</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W+-">W. -P. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Coehlo%2C+N+K">N. K. Coehlo</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K+H">K. H. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Dave%2C+R">R. Dave</a>, <a href="/search/astro-ph?searchtype=author&query=King%2C+S+-">S. -K. King</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+T">T. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lehner%2C+M+J">M. J. Lehner</a>, <a href="/search/astro-ph?searchtype=author&query=Lin%2C+H+-">H. -C. Lin</a>, <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+S+L">S. L. Marshall</a>, <a href="/search/astro-ph?searchtype=author&query=Porrata%2C+R">R. Porrata</a>, <a href="/search/astro-ph?searchtype=author&query=Rice%2C+J+A">J. A. Rice</a>, <a href="/search/astro-ph?searchtype=author&query=Schwamb%2C+M+E">M. E. Schwamb</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+J+-">J. -H. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+S+-">S. -Y. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Wen%2C+C+-">C. -Y. Wen</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+Z+-">Z. -W. Zhang</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="0912.1791v2-abstract-short" style="display: inline;"> We analyzed data accumulated during 2005 and 2006 by the Taiwan-American Occultation Survey (TAOS) in order to detect short-period variable stars (periods of <~ 1 hour) such as delta Scuti. TAOS is designed for the detection of stellar occultation by small-size Kuiper Belt Objects (KBOs) and is operating four 50cm telescopes at an effective cadence of 5Hz. The four telescopes simultaneously moni… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0912.1791v2-abstract-full').style.display = 'inline'; document.getElementById('0912.1791v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0912.1791v2-abstract-full" style="display: none;"> We analyzed data accumulated during 2005 and 2006 by the Taiwan-American Occultation Survey (TAOS) in order to detect short-period variable stars (periods of <~ 1 hour) such as delta Scuti. TAOS is designed for the detection of stellar occultation by small-size Kuiper Belt Objects (KBOs) and is operating four 50cm telescopes at an effective cadence of 5Hz. The four telescopes simultaneously monitor the same patch of the sky in order to reduce false positives. To detect short-period variables, we used the Fast Fourier Transform algorithm (FFT) inasmuch as the data points in TAOS light-curves are evenly spaced. Using FFT, we found 41 short-period variables with amplitudes smaller than a few hundredths of a magnitude and periods of about an hour, which suggest that they are low-amplitude delta Scuti stars (LADS). The light-curves of TAOS delta Scuti stars are accessible online at the Time Series Center website (http://timemachine.iic.harvard.edu) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0912.1791v2-abstract-full').style.display = 'none'; document.getElementById('0912.1791v2-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 December, 2009; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 December, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2009. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0912.1171">arXiv:0912.1171</a> <span> [<a href="https://arxiv.org/pdf/0912.1171">pdf</a>, <a href="https://arxiv.org/ps/0912.1171">ps</a>, <a href="https://arxiv.org/format/0912.1171">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/710/2/1641">10.1088/0004-637X/710/2/1641 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Cold Neptune-Mass Planet OGLE-2007-BLG-368Lb: Cold Neptunes Are Common </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sumi%2C+T">T. Sumi</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+D+P">D. P. Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+I+A">I. A. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">A. Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+V">V. Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Dominik%2C+M">M. Dominik</a>, <a href="/search/astro-ph?searchtype=author&query=Fouqu%C3%A9%2C+P">P. Fouqu茅</a>, <a href="/search/astro-ph?searchtype=author&query=Kubas%2C+D">D. Kubas</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">A. Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Macintosh%2C+B">B. Macintosh</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K">K. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+S">S. Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Skuljan%2C+L">L. Skuljan</a>, <a href="/search/astro-ph?searchtype=author&query=Cassan%2C+A">A. Cassan</a>, <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+T+M">The MOA Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+F">F. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Botzler%2C+C+S">C. S. Botzler</a>, <a href="/search/astro-ph?searchtype=author&query=Fukui%2C+A">A. Fukui</a>, <a href="/search/astro-ph?searchtype=author&query=Furusawa%2C+K">K. Furusawa</a>, <a href="/search/astro-ph?searchtype=author&query=Hearnshaw%2C+J+B">J. B. Hearnshaw</a>, <a href="/search/astro-ph?searchtype=author&query=Itow%2C+Y">Y. Itow</a>, <a href="/search/astro-ph?searchtype=author&query=Kamiya%2C+K">K. Kamiya</a>, <a href="/search/astro-ph?searchtype=author&query=Kilmartin%2C+P+M">P. M. Kilmartin</a>, <a href="/search/astro-ph?searchtype=author&query=Korpela%2C+A">A. Korpela</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="0912.1171v3-abstract-short" style="display: inline;"> We present the discovery of a Neptune-mass planet OGLE-2007-BLG-368Lb with a planet-star mass ratio of q=[9.5 +/- 2.1] x 10^{-5} via gravitational microlensing. The planetary deviation was detected in real-time thanks to the high cadence of the MOA survey, real-time light curve monitoring and intensive follow-up observations. A Bayesian analysis returns the stellar mass and distance at M_l = 0.6… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0912.1171v3-abstract-full').style.display = 'inline'; document.getElementById('0912.1171v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0912.1171v3-abstract-full" style="display: none;"> We present the discovery of a Neptune-mass planet OGLE-2007-BLG-368Lb with a planet-star mass ratio of q=[9.5 +/- 2.1] x 10^{-5} via gravitational microlensing. The planetary deviation was detected in real-time thanks to the high cadence of the MOA survey, real-time light curve monitoring and intensive follow-up observations. A Bayesian analysis returns the stellar mass and distance at M_l = 0.64_{-0.26}^{+0.21} M_\sun and D_l = 5.9_{-1.4}^{+0.9} kpc, respectively, so the mass and separation of the planet are M_p = 20_{-8}^{+7} M_\oplus and a = 3.3_{-0.8}^{+1.4} AU, respectively. This discovery adds another cold Neptune-mass planet to the planetary sample discovered by microlensing, which now comprise four cold Neptune/Super-Earths, five gas giant planets, and another sub-Saturn mass planet whose nature is unclear. The discovery of these ten cold exoplanets by the microlensing method implies that the mass ratio function of cold exoplanets scales as dN_{\rm pl}/d\log q \propto q^{-0.7 +/- 0.2} with a 95% confidence level upper limit of n < -0.35 (where dN_{\rm pl}/d\log q \propto q^n). As microlensing is most sensitive to planets beyond the snow-line, this implies that Neptune-mass planets are at least three times more common than Jupiters in this region at the 95% confidence level. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0912.1171v3-abstract-full').style.display = 'none'; document.getElementById('0912.1171v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 January, 2010; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 December, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2009. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">39 pages, 10 figures, accepted for publication in ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.710:1641-1653,2010 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0912.0201">arXiv:0912.0201</a> <span> [<a href="https://arxiv.org/pdf/0912.0201">pdf</a>, <a href="https://arxiv.org/format/0912.0201">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> LSST Science Book, Version 2.0 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=LSST+Science+Collaboration"> LSST Science Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abell%2C+P+A">Paul A. Abell</a>, <a href="/search/astro-ph?searchtype=author&query=Allison%2C+J">Julius Allison</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+S+F">Scott F. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Andrew%2C+J+R">John R. Andrew</a>, <a href="/search/astro-ph?searchtype=author&query=Angel%2C+J+R+P">J. Roger P. Angel</a>, <a href="/search/astro-ph?searchtype=author&query=Armus%2C+L">Lee Armus</a>, <a href="/search/astro-ph?searchtype=author&query=Arnett%2C+D">David Arnett</a>, <a href="/search/astro-ph?searchtype=author&query=Asztalos%2C+S+J">S. J. Asztalos</a>, <a href="/search/astro-ph?searchtype=author&query=Axelrod%2C+T+S">Tim S. Axelrod</a>, <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+S">Stephen Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Ballantyne%2C+D+R">D. R. Ballantyne</a>, <a href="/search/astro-ph?searchtype=author&query=Bankert%2C+J+R">Justin R. Bankert</a>, <a href="/search/astro-ph?searchtype=author&query=Barkhouse%2C+W+A">Wayne A. Barkhouse</a>, <a href="/search/astro-ph?searchtype=author&query=Barr%2C+J+D">Jeffrey D. Barr</a>, <a href="/search/astro-ph?searchtype=author&query=Barrientos%2C+L+F">L. Felipe Barrientos</a>, <a href="/search/astro-ph?searchtype=author&query=Barth%2C+A+J">Aaron J. Barth</a>, <a href="/search/astro-ph?searchtype=author&query=Bartlett%2C+J+G">James G. Bartlett</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+A+C">Andrew C. Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Becla%2C+J">Jacek Becla</a>, <a href="/search/astro-ph?searchtype=author&query=Beers%2C+T+C">Timothy C. Beers</a>, <a href="/search/astro-ph?searchtype=author&query=Bernstein%2C+J+P">Joseph P. Bernstein</a>, <a href="/search/astro-ph?searchtype=author&query=Biswas%2C+R">Rahul Biswas</a>, <a href="/search/astro-ph?searchtype=author&query=Blanton%2C+M+R">Michael R. Blanton</a>, <a href="/search/astro-ph?searchtype=author&query=Bloom%2C+J+S">Joshua S. Bloom</a> , et al. (223 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0912.0201v1-abstract-short" style="display: inline;"> A survey that can cover the sky in optical bands over wide fields to faint magnitudes with a fast cadence will enable many of the exciting science opportunities of the next decade. The Large Synoptic Survey Telescope (LSST) will have an effective aperture of 6.7 meters and an imaging camera with field of view of 9.6 deg^2, and will be devoted to a ten-year imaging survey over 20,000 deg^2 south… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0912.0201v1-abstract-full').style.display = 'inline'; document.getElementById('0912.0201v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0912.0201v1-abstract-full" style="display: none;"> A survey that can cover the sky in optical bands over wide fields to faint magnitudes with a fast cadence will enable many of the exciting science opportunities of the next decade. The Large Synoptic Survey Telescope (LSST) will have an effective aperture of 6.7 meters and an imaging camera with field of view of 9.6 deg^2, and will be devoted to a ten-year imaging survey over 20,000 deg^2 south of +15 deg. Each pointing will be imaged 2000 times with fifteen second exposures in six broad bands from 0.35 to 1.1 microns, to a total point-source depth of r~27.5. The LSST Science Book describes the basic parameters of the LSST hardware, software, and observing plans. The book discusses educational and outreach opportunities, then goes on to describe a broad range of science that LSST will revolutionize: mapping the inner and outer Solar System, stellar populations in the Milky Way and nearby galaxies, the structure of the Milky Way disk and halo and other objects in the Local Volume, transient and variable objects both at low and high redshift, and the properties of normal and active galaxies at low and high redshift. It then turns to far-field cosmological topics, exploring properties of supernovae to z~1, strong and weak lensing, the large-scale distribution of galaxies and baryon oscillations, and how these different probes may be combined to constrain cosmological models and the physics of dark energy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0912.0201v1-abstract-full').style.display = 'none'; document.getElementById('0912.0201v1-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 December, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2009. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">596 pages. Also available at full resolution at http://www.lsst.org/lsst/scibook</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0911.2706">arXiv:0911.2706</a> <span> [<a href="https://arxiv.org/pdf/0911.2706">pdf</a>, <a href="https://arxiv.org/format/0911.2706">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/713/2/837">10.1088/0004-637X/713/2/837 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Masses and Orbital Constraints for the OGLE-2006-BLG-109Lb,c Jupiter/Saturn Analog Planetary System </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+D+P">D. P. Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Rhie%2C+S+H">S. H. Rhie</a>, <a href="/search/astro-ph?searchtype=author&query=Nikolaev%2C+S">S. Nikolaev</a>, <a href="/search/astro-ph?searchtype=author&query=Gaudi%2C+B+S">B. S. Gaudi</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">A. Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">A. Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Christie%2C+G+W">G. W. Christie</a>, <a href="/search/astro-ph?searchtype=author&query=Maoz%2C+D">D. Maoz</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+S">S. Dong</a>, <a href="/search/astro-ph?searchtype=author&query=McCormick%2C+J">J. McCormick</a>, <a href="/search/astro-ph?searchtype=author&query=Szymanski%2C+M+K">M. K. Szymanski</a>, <a href="/search/astro-ph?searchtype=author&query=Tristram%2C+P+J">P. J. Tristram</a>, <a href="/search/astro-ph?searchtype=author&query=Macintosh%2C+B">B. Macintosh</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K+H">K. H. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Kubiak%2C+M">M. Kubiak</a>, <a href="/search/astro-ph?searchtype=author&query=Pietrzynski%2C+G">G. Pietrzynski</a>, <a href="/search/astro-ph?searchtype=author&query=Soszynski%2C+I">I. Soszynski</a>, <a href="/search/astro-ph?searchtype=author&query=Szewczyk%2C+O">O. Szewczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">K. Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Wyrzykowski%2C+L">L. Wyrzykowski</a>, <a href="/search/astro-ph?searchtype=author&query=DePoy%2C+D+L">D. L. DePoy</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">C. Han</a>, <a href="/search/astro-ph?searchtype=author&query=Kaspi%2C+S">S. Kaspi</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C+-">C. -U. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Mallia%2C+F">F. Mallia</a> , et al. (48 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="0911.2706v4-abstract-short" style="display: inline;"> We present a new analysis of the Jupiter+Saturn analog system, OGLE-2006-BLG-109Lb,c, which was the first double planet system discovered with the gravitational microlensing method. This is the only multi-planet system discovered by any method with measured masses for the star and both planets. In addition to the signatures of two planets, this event also exhibits a microlensing parallax signature… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0911.2706v4-abstract-full').style.display = 'inline'; document.getElementById('0911.2706v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0911.2706v4-abstract-full" style="display: none;"> We present a new analysis of the Jupiter+Saturn analog system, OGLE-2006-BLG-109Lb,c, which was the first double planet system discovered with the gravitational microlensing method. This is the only multi-planet system discovered by any method with measured masses for the star and both planets. In addition to the signatures of two planets, this event also exhibits a microlensing parallax signature and finite source effects that provide a direct measure of the masses of the star and planets, and the expected brightness of the host star is confirmed by Keck AO imaging, yielding masses of M_* = 0.51(+0.05-0.04) M_sun, M_b = 231+-19 M_earth, M_c = 86+-7 M_earth. The Saturn-analog planet in this system had a planetary light curve deviation that lasted for 11 days, and as a result, the effects of the orbital motion are visible in the microlensing light curve. We find that four of the six orbital parameters are tightly constrained and that a fifth parameter, the orbital acceleration, is weakly constrained. No orbital information is available for the Jupiter-analog planet, but its presence helps to constrain the orbital motion of the Saturn-analog planet. Assuming co-planar orbits, we find an orbital eccentricity of eccentricity = 0.15 (+0.17-0.10) and an orbital inclination of i = 64 (+4-7) deg. The 95% confidence level lower limit on the inclination of i > 49 deg. implies that this planetary system can be detected and studied via radial velocity measurements using a telescope of >30m aperture. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0911.2706v4-abstract-full').style.display = 'none'; document.getElementById('0911.2706v4-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 June, 2010; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 November, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2009. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">48 pages including 10 figures, to be published in ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.713:837-855,2010 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0911.2002">arXiv:0911.2002</a> <span> [<a href="https://arxiv.org/pdf/0911.2002">pdf</a>, <a href="https://arxiv.org/ps/0911.2002">ps</a>, <a href="https://arxiv.org/format/0911.2002">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/729/2/88">10.1088/0004-637X/729/2/88 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Pushing the Boundaries of Conventional Core-Collapse Supernovae: The Extremely Energetic Supernova SN 2003ma </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rest%2C+A">A. Rest</a>, <a href="/search/astro-ph?searchtype=author&query=Foley%2C+R+J">R. J. Foley</a>, <a href="/search/astro-ph?searchtype=author&query=Gezari%2C+S">S. Gezari</a>, <a href="/search/astro-ph?searchtype=author&query=Narayan%2C+G">G. Narayan</a>, <a href="/search/astro-ph?searchtype=author&query=Draine%2C+B">B. Draine</a>, <a href="/search/astro-ph?searchtype=author&query=Olsen%2C+K">K. Olsen</a>, <a href="/search/astro-ph?searchtype=author&query=Huber%2C+M">M. Huber</a>, <a href="/search/astro-ph?searchtype=author&query=Matheson%2C+T">T. Matheson</a>, <a href="/search/astro-ph?searchtype=author&query=Garg%2C+A">A. Garg</a>, <a href="/search/astro-ph?searchtype=author&query=Welch%2C+D+L">D. L. Welch</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+A+C">A. C. Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Challis%2C+P">P. Challis</a>, <a href="/search/astro-ph?searchtype=author&query=Clocchiatti%2C+A">A. Clocchiatti</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K+H">K. H. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Damke%2C+G">G. Damke</a>, <a href="/search/astro-ph?searchtype=author&query=Meixner%2C+M">M. Meixner</a>, <a href="/search/astro-ph?searchtype=author&query=Miknaitis%2C+G">G. Miknaitis</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Morelli%2C+L">L. Morelli</a>, <a href="/search/astro-ph?searchtype=author&query=Nikolaev%2C+S">S. Nikolaev</a>, <a href="/search/astro-ph?searchtype=author&query=Pignata%2C+G">G. Pignata</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+J+L">J. L. Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+R+C">R. C. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Stubbs%2C+C">C. Stubbs</a>, <a href="/search/astro-ph?searchtype=author&query=Suntzeff%2C+N+B">N. B. Suntzeff</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="0911.2002v3-abstract-short" style="display: inline;"> We report the discovery of a supernova (SN) with the highest apparent energy output to date and conclude that it represents an extreme example of the Type IIn subclass. The SN, which was discovered behind the Large Magellanic Cloud at z = 0.289 by the SuperMACHO microlensing survey, peaked at M_R = -21.5 mag and only declined by 2.9 mag over 4.7 years after the peak. Over this period, SN 2003ma ha… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0911.2002v3-abstract-full').style.display = 'inline'; document.getElementById('0911.2002v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0911.2002v3-abstract-full" style="display: none;"> We report the discovery of a supernova (SN) with the highest apparent energy output to date and conclude that it represents an extreme example of the Type IIn subclass. The SN, which was discovered behind the Large Magellanic Cloud at z = 0.289 by the SuperMACHO microlensing survey, peaked at M_R = -21.5 mag and only declined by 2.9 mag over 4.7 years after the peak. Over this period, SN 2003ma had an integrated bolometric luminosity of 4 x 10^51 ergs, more than any other SN to date. The radiated energy is close to the limit allowed by conventional core-collapse explosions. Optical spectra reveal that SN 2003ma has persistent single-peaked intermediate-width hydrogen lines, a signature of interaction between the SN and a dense circumstellar medium. The light curves show further evidence for circumstellar interaction, including a long plateau with a shape very similar to the classic SN IIn 1988Z -- however, SN 2003ma is ten times more luminous at all epochs. The fast velocity measured for the intermediate-width H_alpha component (~6000 km/s) points towards an extremely energetic explosion (> 10^52 ergs), which imparts a faster blast-wave speed to the post-shock material and a higher luminosity from the interaction than is observed in typical SNe IIn. Mid-infrared observations of SN 2003ma suggest an infrared light echo is produced by normal interstellar dust at a distance ~0.5 pc from the SN. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0911.2002v3-abstract-full').style.display = 'none'; document.getElementById('0911.2002v3-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 December, 2010; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 November, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2009. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 15 figures, accepted for publication in ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.729:88,2011 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0910.5282">arXiv:0910.5282</a> <span> [<a href="https://arxiv.org/pdf/0910.5282">pdf</a>, <a href="https://arxiv.org/ps/0910.5282">ps</a>, <a href="https://arxiv.org/format/0910.5282">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-6256/138/6/1893">10.1088/0004-6256/138/6/1893 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Upper Limits on the Number of Small Bodies in Sedna-Like Orbits by the TAOS Project </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wang%2C+J+-">J. -H. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Lehner%2C+M+J">M. J. Lehner</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+Z+-">Z. -W. Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Bianco%2C+F+B">F. B. Bianco</a>, <a href="/search/astro-ph?searchtype=author&query=Alcock%2C+C">C. Alcock</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W+-">W. -P. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Axelrod%2C+T">T. Axelrod</a>, <a href="/search/astro-ph?searchtype=author&query=Byun%2C+Y+-">Y. -I. Byun</a>, <a href="/search/astro-ph?searchtype=author&query=Coehlo%2C+N+K">N. K. Coehlo</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K+H">K. H. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Dave%2C+R">R. Dave</a>, <a href="/search/astro-ph?searchtype=author&query=de+Pater%2C+I">I. de Pater</a>, <a href="/search/astro-ph?searchtype=author&query=Porrata%2C+R">R. Porrata</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D+-">D. -W. Kim</a>, <a href="/search/astro-ph?searchtype=author&query=King%2C+S+-">S. -K. King</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+T">T. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lin%2C+H+-">H. -C. Lin</a>, <a href="/search/astro-ph?searchtype=author&query=Lissauer%2C+J+J">J. J. Lissauer</a>, <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+S+L">S. L. Marshall</a>, <a href="/search/astro-ph?searchtype=author&query=Protopapas%2C+P">P. Protopapas</a>, <a href="/search/astro-ph?searchtype=author&query=Rice%2C+J+A">J. A. Rice</a>, <a href="/search/astro-ph?searchtype=author&query=Schwamb%2C+M+E">M. E. Schwamb</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+S+-">S. -Y. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Wen%2C+C+-">C. -Y. Wen</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="0910.5282v1-abstract-short" style="display: inline;"> We present the results of a search for occultation events by objects at distances between 100 and 1000 AU in lightcurves from the Taiwanese-American Occultation Survey (TAOS). We searched for consecutive, shallow flux reductions in the stellar lightcurves obtained by our survey between 7 February 2005 and 31 December 2006 with a total of $\sim4.5\times10^{9}$ three-telescope simultaneous photome… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0910.5282v1-abstract-full').style.display = 'inline'; document.getElementById('0910.5282v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0910.5282v1-abstract-full" style="display: none;"> We present the results of a search for occultation events by objects at distances between 100 and 1000 AU in lightcurves from the Taiwanese-American Occultation Survey (TAOS). We searched for consecutive, shallow flux reductions in the stellar lightcurves obtained by our survey between 7 February 2005 and 31 December 2006 with a total of $\sim4.5\times10^{9}$ three-telescope simultaneous photometric measurements. No events were detected, allowing us to set upper limits on the number density as a function of size and distance of objects in Sedna-like orbits, using simple models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0910.5282v1-abstract-full').style.display = 'none'; document.getElementById('0910.5282v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 October, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2009. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 13 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/0907.5421">arXiv:0907.5421</a> <span> [<a href="https://arxiv.org/pdf/0907.5421">pdf</a>, <a href="https://arxiv.org/ps/0907.5421">ps</a>, <a href="https://arxiv.org/format/0907.5421">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/713/2/1167">10.1088/0004-637X/713/2/1167 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Lower bounds on photometric redshift errors from Type Ia supernovae templates </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Asztalos%2C+S">S. Asztalos</a>, <a href="/search/astro-ph?searchtype=author&query=Nikolaev%2C+S">S. Nikolaev</a>, <a href="/search/astro-ph?searchtype=author&query=de+Vries%2C+W">W. de Vries</a>, <a href="/search/astro-ph?searchtype=author&query=Olivier%2C+S">S. Olivier</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K">K. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+L">L. Wang</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="0907.5421v1-abstract-short" style="display: inline;"> Cosmology with Type Ia supernovae heretofore has required extensive spectroscopic follow-up to establish a redshift. Though tolerable at the present discovery rate, the next generation of ground-based all-sky survey instruments will render this approach unsustainable. Photometry-based redshift determination is a viable alternative, but introduces non-negligible errors that ultimately degrade the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0907.5421v1-abstract-full').style.display = 'inline'; document.getElementById('0907.5421v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0907.5421v1-abstract-full" style="display: none;"> Cosmology with Type Ia supernovae heretofore has required extensive spectroscopic follow-up to establish a redshift. Though tolerable at the present discovery rate, the next generation of ground-based all-sky survey instruments will render this approach unsustainable. Photometry-based redshift determination is a viable alternative, but introduces non-negligible errors that ultimately degrade the ability to discriminate between competing cosmologies. We present a strictly template-based photometric redshift estimator and compute redshift reconstruction errors in the presence of photometry and statistical errors. With reasonable assumptions for a cadence and supernovae distribution, these redshift errors are combined with systematic errors and propagated using the Fisher matrix formalism to derive lower bounds on the joint errors in $惟_w$ and $惟_w'$ relevant to the next generation of ground-based all-sky survey. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0907.5421v1-abstract-full').style.display = 'none'; document.getElementById('0907.5421v1-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 July, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2009. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 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/0907.3471">arXiv:0907.3471</a> <span> [<a href="https://arxiv.org/pdf/0907.3471">pdf</a>, <a href="https://arxiv.org/ps/0907.3471">ps</a>, <a href="https://arxiv.org/format/0907.3471">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> <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/10.1051/0004-6361/200912923">10.1051/0004-6361/200912923 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Mass measurement of a single unseen star and planetary detection efficiency for OGLE 2007-BLG-050 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Batista%2C+V">V. Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+S">Subo Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">A. Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Beaulieu%2C+J+P">J. P. Beaulieu</a>, <a href="/search/astro-ph?searchtype=author&query=Cassan%2C+A">A. Cassan</a>, <a href="/search/astro-ph?searchtype=author&query=Christie%2C+G+W">G. W. Christie</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">C. Han</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">A. Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+W">W. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=DePoy%2C+D+L">D. L. DePoy</a>, <a href="/search/astro-ph?searchtype=author&query=Gal-Yam%2C+A">A. Gal-Yam</a>, <a href="/search/astro-ph?searchtype=author&query=Gaudi%2C+B+S">B. S. Gaudi</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+B">B. Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Kaspi%2C+S">S. Kaspi</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C+U">C. U. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Maoz%2C+D">D. Maoz</a>, <a href="/search/astro-ph?searchtype=author&query=McCormick%2C+J">J. McCormick</a>, <a href="/search/astro-ph?searchtype=author&query=McGreer%2C+I">I. McGreer</a>, <a href="/search/astro-ph?searchtype=author&query=Monard%2C+B">B. Monard</a>, <a href="/search/astro-ph?searchtype=author&query=Natusch%2C+T">T. Natusch</a>, <a href="/search/astro-ph?searchtype=author&query=Ofek%2C+E">E. Ofek</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B+-">B. -G. Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">R. W. Pogge</a>, <a href="/search/astro-ph?searchtype=author&query=Polishook%2C+D">D. Polishook</a>, <a href="/search/astro-ph?searchtype=author&query=Shporer%2C+A">A. Shporer</a> , et al. (71 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="0907.3471v3-abstract-short" style="display: inline;"> We analyze OGLE-2007-BLG-050, a high magnification microlensing event (A ~ 432) whose peak occurred on 2 May, 2007, with pronounced finite-source and parallax effects. We compute planet detection efficiencies for this event in order to determine its sensitivity to the presence of planets around the lens star. Both finite-source and parallax effects permit a measurement of the angular Einstein ra… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0907.3471v3-abstract-full').style.display = 'inline'; document.getElementById('0907.3471v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0907.3471v3-abstract-full" style="display: none;"> We analyze OGLE-2007-BLG-050, a high magnification microlensing event (A ~ 432) whose peak occurred on 2 May, 2007, with pronounced finite-source and parallax effects. We compute planet detection efficiencies for this event in order to determine its sensitivity to the presence of planets around the lens star. Both finite-source and parallax effects permit a measurement of the angular Einstein radius 胃_E = 0.48 +/- 0.01 mas and the parallax 蟺_E = 0.12 +/- 0.03, leading to an estimate of the lens mass M = 0.50 +/- 0.14 M_Sun and its distance to the observer D_L = 5.5 +/- 0.4 kpc. This is only the second determination of a reasonably precise (<30%) mass estimate for an isolated unseen object, using any method. This allows us to calculate the planetary detection efficiency in physical units (r_\perp, m_p), where r_\perp is the projected planet-star separation and m_p is the planet mass. When computing planet detection efficiency, we did not find any planetary signature and our detection efficiency results reveal significant sensitivity to Neptune-mass planets, and to a lesser extent Earth-mass planets in some configurations. Indeed, Jupiter and Neptune-mass planets are excluded with a high confidence for a large projected separation range between the planet and the lens star, respectively [0.6 - 10] and [1.4 - 4] AU, and Earth-mass planets are excluded with a 10% confidence in the lensing zone, i.e. [1.8 - 3.1] AU. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0907.3471v3-abstract-full').style.display = 'none'; document.getElementById('0907.3471v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 July, 2009; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 July, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2009. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 23 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2009A&A...508..467B </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0905.1965">arXiv:0905.1965</a> <span> [<a href="https://arxiv.org/pdf/0905.1965">pdf</a>, <a href="https://arxiv.org/format/0905.1965">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The Synoptic All-Sky Infrared (SASIR) Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bloom%2C+J+S">Joshua S. Bloom</a>, <a href="/search/astro-ph?searchtype=author&query=Prochaska%2C+J+X">J. Xavier Prochaska</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+W">William Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez%2C+J+J">J. Jes煤s Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Ram%C3%ADrez-Ruiz%2C+E">Enrico Ram铆rez-Ruiz</a>, <a href="/search/astro-ph?searchtype=author&query=Bolte%2C+M">Michael Bolte</a>, <a href="/search/astro-ph?searchtype=author&query=Franco%2C+J">Jos茅 Franco</a>, <a href="/search/astro-ph?searchtype=author&query=Guichard%2C+J">Jos茅 Guichard</a>, <a href="/search/astro-ph?searchtype=author&query=Carrami%C3%B1ana%2C+A">Alberto Carrami帽ana</a>, <a href="/search/astro-ph?searchtype=author&query=Strittmatter%2C+P">Peter Strittmatter</a>, <a href="/search/astro-ph?searchtype=author&query=Avila-Reese%2C+V">Vladimir Avila-Reese</a>, <a href="/search/astro-ph?searchtype=author&query=Bernstein%2C+R">Rebecca Bernstein</a>, <a href="/search/astro-ph?searchtype=author&query=Bigelow%2C+B">Bruce Bigelow</a>, <a href="/search/astro-ph?searchtype=author&query=Brodwin%2C+M">Mark Brodwin</a>, <a href="/search/astro-ph?searchtype=author&query=Burgasser%2C+A">Adam Burgasser</a>, <a href="/search/astro-ph?searchtype=author&query=Butler%2C+N">Nat Butler</a>, <a href="/search/astro-ph?searchtype=author&query=Ch%C3%A1vez%2C+M">Miguel Ch谩vez</a>, <a href="/search/astro-ph?searchtype=author&query=Cobb%2C+B">Bethany Cobb</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K">Kem Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Cruz-Gonz%C3%A1lez%2C+I">Irene Cruz-Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=de+Diego%2C+J+A">Jos茅 Antonio de Diego</a>, <a href="/search/astro-ph?searchtype=author&query=Farah%2C+A">Alejandro Farah</a>, <a href="/search/astro-ph?searchtype=author&query=Georgiev%2C+L">Leonid Georgiev</a>, <a href="/search/astro-ph?searchtype=author&query=Girard%2C+J">Julien Girard</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez-Toledo%2C+H">Hector Hern谩ndez-Toledo</a> , et al. (20 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="0905.1965v2-abstract-short" style="display: inline;"> We are proposing to conduct a multicolor, synoptic infrared (IR) imaging survey of the Northern sky with a new, dedicated 6.5-meter telescope at San Pedro M谩rtir (SPM) Observatory. This initiative is being developed in partnership with astronomy institutions in Mexico and the University of California. The 4-year, dedicated survey, planned to begin in 2017, will reach more than 100 times deeper t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0905.1965v2-abstract-full').style.display = 'inline'; document.getElementById('0905.1965v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0905.1965v2-abstract-full" style="display: none;"> We are proposing to conduct a multicolor, synoptic infrared (IR) imaging survey of the Northern sky with a new, dedicated 6.5-meter telescope at San Pedro M谩rtir (SPM) Observatory. This initiative is being developed in partnership with astronomy institutions in Mexico and the University of California. The 4-year, dedicated survey, planned to begin in 2017, will reach more than 100 times deeper than 2MASS. The Synoptic All-Sky Infrared (SASIR) Survey will reveal the missing sample of faint red dwarf stars in the local solar neighborhood, and the unprecedented sensitivity over such a wide field will result in the discovery of thousands of z ~ 7 quasars (and reaching to z > 10), allowing detailed study (in concert with JWST and Giant Segmented Mirror Telescopes) of the timing and the origin(s) of reionization. As a time-domain survey, SASIR will reveal the dynamic infrared universe, opening new phase space for discovery. Synoptic observations of over 10^6 supernovae and variable stars will provide better distance measures than optical studies alone. SASIR also provides significant synergy with other major Astro2010 facilities, improving the overall scientific return of community investments. Compared to optical-only measurements, IR colors vastly improve photometric redshifts to z ~ 4, enhancing dark energy and dark matter surveys based on weak lensing and baryon oscillations. The wide field and ToO capabilities will enable a connection of the gravitational wave and neutrino universe - with events otherwise poorly localized on the sky - to transient electromagnetic phenomena. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0905.1965v2-abstract-full').style.display = 'none'; document.getElementById('0905.1965v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 July, 2009; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 May, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2009. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Revised version of submitted whitepaper to the "Optical and IR Astronomy from the Ground" Program Prioritization Panel of the Astro2010 Decadal Survey; 23 pages</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0902.3000">arXiv:0902.3000</a> <span> [<a href="https://arxiv.org/pdf/0902.3000">pdf</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> <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"> A Census of Exoplanets in Orbits Beyond 0.5 AU via Space-based Microlensing </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+D+P">David P. Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Beaulieu%2C+J+-">J. -P. Beaulieu</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+I">I. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+E">E. Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K">K. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Friedman%2C+S">S. Friedman</a>, <a href="/search/astro-ph?searchtype=author&query=Gaudi%2C+B+S">B. S. Gaudi</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">A. Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Jenkins%2C+J">J. Jenkins</a>, <a href="/search/astro-ph?searchtype=author&query=Kimble%2C+R">R. Kimble</a>, <a href="/search/astro-ph?searchtype=author&query=Lin%2C+D">D. Lin</a>, <a href="/search/astro-ph?searchtype=author&query=Mather%2C+J">J. Mather</a>, <a href="/search/astro-ph?searchtype=author&query=Rich%2C+M">M. Rich</a>, <a href="/search/astro-ph?searchtype=author&query=Sahu%2C+K">K. Sahu</a>, <a href="/search/astro-ph?searchtype=author&query=Sumi%2C+T">T. Sumi</a>, <a href="/search/astro-ph?searchtype=author&query=Tenerelli%2C+D">D. Tenerelli</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">A. Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Yock%2C+P">P. Yock</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="0902.3000v1-abstract-short" style="display: inline;"> A space-based gravitational microlensing exoplanet survey will provide a statistical census of exoplanets with masses greater than 0.1 Earth-masses and orbital separations ranging from 0.5AU to infinity. This includes analogs to all the Solar System's planets except for Mercury, as well as most types of planets predicted by planet formation theories. Such a survey will provide results on the fre… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0902.3000v1-abstract-full').style.display = 'inline'; document.getElementById('0902.3000v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0902.3000v1-abstract-full" style="display: none;"> A space-based gravitational microlensing exoplanet survey will provide a statistical census of exoplanets with masses greater than 0.1 Earth-masses and orbital separations ranging from 0.5AU to infinity. This includes analogs to all the Solar System's planets except for Mercury, as well as most types of planets predicted by planet formation theories. Such a survey will provide results on the frequency of planets around all types of stars except those with short lifetimes. Close-in planets with separations < 0.5 AU are invisible to a space-based microlensing survey, but these can be found by Kepler. Other methods, including ground-based microlensing, cannot approach the comprehensive statistics on the mass and semi-major axis distribution of extrasolar planets that a space-based microlensing survey will provide. The terrestrial planet sensitivity of a ground-based microlensing survey is limited to the vicinity of the Einstein radius at 2-3 AU, and space-based imaging is needed to identify and determine the mass of the planetary host stars for the vast majority of planets discovered by microlensing. Thus, a space-based microlensing survey is likely to be the only way to gain a comprehensive understanding of the architecture of planetary systems, which is needed to understand planet formation and habitability. The proposed Microlensing Planet Finder (MPF) mission is an example of a space-based microlensing survey that can accomplish these objectives with proven technology and a cost of under $300 million (excluding launch vehicle). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0902.3000v1-abstract-full').style.display = 'none'; document.getElementById('0902.3000v1-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 February, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2009. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages (including cover), White Paper to the Astro2010 PSF Science Frontier Panel</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0902.2213">arXiv:0902.2213</a> <span> [<a href="https://arxiv.org/pdf/0902.2213">pdf</a>, <a href="https://arxiv.org/format/0902.2213">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> The MACHO Project HST Follow-Up: The Large Magellanic Cloud Microlensing Source Stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Nelson%2C+C+A">C. A. Nelson</a>, <a href="/search/astro-ph?searchtype=author&query=Drake%2C+A+J">A. J. Drake</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K+H">K. H. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+D+P">D. P. Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Popowski%2C+P">P. Popowski</a>, <a href="/search/astro-ph?searchtype=author&query=Dalal%2C+N">N. Dalal</a>, <a href="/search/astro-ph?searchtype=author&query=Nikolaev%2C+S">S. Nikolaev</a>, <a href="/search/astro-ph?searchtype=author&query=Alcock%2C+C">C. Alcock</a>, <a href="/search/astro-ph?searchtype=author&query=Axelrod%2C+T+S">T. S. Axelrod</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+A+C">A. C. Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Freeman%2C+K+C">K. C. Freeman</a>, <a href="/search/astro-ph?searchtype=author&query=Geha%2C+M">M. Geha</a>, <a href="/search/astro-ph?searchtype=author&query=Griest%2C+K">K. Griest</a>, <a href="/search/astro-ph?searchtype=author&query=Keller%2C+S+C">S. C. Keller</a>, <a href="/search/astro-ph?searchtype=author&query=Lehner%2C+M+J">M. J. Lehner</a>, <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+S+L">S. L. Marshall</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Pratt%2C+M+R">M. R. Pratt</a>, <a href="/search/astro-ph?searchtype=author&query=Quinn%2C+P+J">P. J. Quinn</a>, <a href="/search/astro-ph?searchtype=author&query=Stubbs%2C+C+W">C. W. Stubbs</a>, <a href="/search/astro-ph?searchtype=author&query=Sutherland%2C+W">W. Sutherland</a>, <a href="/search/astro-ph?searchtype=author&query=Tomaney%2C+A+B">A. B. Tomaney</a>, <a href="/search/astro-ph?searchtype=author&query=Vandehei%2C+T">T. Vandehei</a>, <a href="/search/astro-ph?searchtype=author&query=Welch%2C+D">D. Welch</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="0902.2213v1-abstract-short" style="display: inline;"> We present Hubble Space Telescope (HST) WFPC2 photometry of 13 microlensed source stars from the 5.7 year Large Magellanic Cloud (LMC) survey conducted by the MACHO Project. The microlensing source stars are identified by deriving accurate centroids in the ground-based MACHO images using difference image analysis (DIA) and then transforming the DIA coordinates to the HST frame. None of these sou… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0902.2213v1-abstract-full').style.display = 'inline'; document.getElementById('0902.2213v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0902.2213v1-abstract-full" style="display: none;"> We present Hubble Space Telescope (HST) WFPC2 photometry of 13 microlensed source stars from the 5.7 year Large Magellanic Cloud (LMC) survey conducted by the MACHO Project. The microlensing source stars are identified by deriving accurate centroids in the ground-based MACHO images using difference image analysis (DIA) and then transforming the DIA coordinates to the HST frame. None of these sources is coincident with a background galaxy, which rules out the possibility that the MACHO LMC microlensing sample is contaminated with misidentified supernovae or AGN in galaxies behind the LMC. This supports the conclusion that the MACHO LMC microlensing sample has only a small amount of contamination due to non-microlensing forms of variability. We compare the WFPC2 source star magnitudes with the lensed flux predictions derived from microlensing fits to the light curve data. In most cases the source star brightness is accurately predicted. Finally, we develop a statistic which constrains the location of the Large Magellanic Cloud (LMC) microlensing source stars with respect to the distributions of stars and dust in the LMC and compare this to the predictions of various models of LMC microlensing. This test excludes at > 90% confidence level models where more than 80% of the source stars lie behind the LMC. Exotic models that attempt to explain the excess LMC microlensing optical depth seen by MACHO with a population of background sources are disfavored or excluded by this test. Models in which most of the lenses reside in a halo or spheroid distribution associated with either the Milky Way or the LMC are consistent which these data, but LMC halo or spheroid models are favored by the combined MACHO and EROS microlensing results. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0902.2213v1-abstract-full').style.display = 'none'; document.getElementById('0902.2213v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 February, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2009. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages with 10 included PDF figures, submitted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0902.1527">arXiv:0902.1527</a> <span> [<a href="https://arxiv.org/pdf/0902.1527">pdf</a>, <a href="https://arxiv.org/ps/0902.1527">ps</a>, <a href="https://arxiv.org/format/0902.1527">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.asr.2012.09.019">10.1016/j.asr.2012.09.019 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Astro2010 Decadal Survey Whitepaper: Coordinated Science in the Gravitational and Electromagnetic Skies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bloom%2C+J+S">Joshua S. Bloom</a>, <a href="/search/astro-ph?searchtype=author&query=Holz%2C+D+E">Daniel E. Holz</a>, <a href="/search/astro-ph?searchtype=author&query=Hughes%2C+S+A">Scott A. Hughes</a>, <a href="/search/astro-ph?searchtype=author&query=Menou%2C+K">Kristen Menou</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+A">Allan Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+S+F">Scott F. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+A">Andy Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Bower%2C+G+C">Geoffrey C. Bower</a>, <a href="/search/astro-ph?searchtype=author&query=Brandt%2C+N">Niel Brandt</a>, <a href="/search/astro-ph?searchtype=author&query=Cobb%2C+B">Bethany Cobb</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K">Kem Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Corsi%2C+A">Alessandra Corsi</a>, <a href="/search/astro-ph?searchtype=author&query=Covino%2C+S">Stefano Covino</a>, <a href="/search/astro-ph?searchtype=author&query=Fox%2C+D">Derek Fox</a>, <a href="/search/astro-ph?searchtype=author&query=Fruchter%2C+A">Andrew Fruchter</a>, <a href="/search/astro-ph?searchtype=author&query=Fryer%2C+C">Chris Fryer</a>, <a href="/search/astro-ph?searchtype=author&query=Grindlay%2C+J">Jonathan Grindlay</a>, <a href="/search/astro-ph?searchtype=author&query=Hartmann%2C+D">Dieter Hartmann</a>, <a href="/search/astro-ph?searchtype=author&query=Haiman%2C+Z">Zoltan Haiman</a>, <a href="/search/astro-ph?searchtype=author&query=Kocsis%2C+B">Bence Kocsis</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+L">Lynne Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Loeb%2C+A">Abraham Loeb</a>, <a href="/search/astro-ph?searchtype=author&query=Marka%2C+S">Szabolcs Marka</a>, <a href="/search/astro-ph?searchtype=author&query=Metzger%2C+B">Brian Metzger</a>, <a href="/search/astro-ph?searchtype=author&query=Nakar%2C+E">Ehud Nakar</a> , et al. (15 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="0902.1527v1-abstract-short" style="display: inline;"> It is widely expected that the coming decade will witness the first direct detection of gravitational waves (GWs). The ground-based LIGO and Virgo GW observatories are being upgraded to advanced sensitivity, and are expected to observe a significant binary merger rate. The launch of The Laser Interferometer Space Antenna (LISA) would extend the GW window to low frequencies, opening new vistas on… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0902.1527v1-abstract-full').style.display = 'inline'; document.getElementById('0902.1527v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0902.1527v1-abstract-full" style="display: none;"> It is widely expected that the coming decade will witness the first direct detection of gravitational waves (GWs). The ground-based LIGO and Virgo GW observatories are being upgraded to advanced sensitivity, and are expected to observe a significant binary merger rate. The launch of The Laser Interferometer Space Antenna (LISA) would extend the GW window to low frequencies, opening new vistas on dynamical processes involving massive (M >~ 10^5 M_Sun) black holes. GW events are likely to be accompanied by electromagnetic (EM) counterparts and, since information carried electromagnetically is complementary to that carried gravitationally, a great deal can be learned about an event and its environment if it becomes possible to measure both forms of radiation in concert. Measurements of this kind will mark the dawn of trans-spectral astrophysics, bridging two distinct spectral bands of information. The aim of this whitepaper is to articulate future directions in both theory and observation that are likely to impact broad astrophysical inquiries of general interest. What will EM observations reflect on the nature and diversity of GW sources? Can GW sources be exploited as complementary probes of cosmology? What cross-facility coordination will expand the science returns of gravitational and electromagnetic observations? <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0902.1527v1-abstract-full').style.display = 'none'; document.getElementById('0902.1527v1-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 February, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2009. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages (plus one coverpage), submitted to the US Astro2010 Decadal Survey. This is a living document, with updates expected to be posted to this archive. Those interested in contributing should contact J. S. Bloom</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0901.2318">arXiv:0901.2318</a> <span> [<a href="https://arxiv.org/pdf/0901.2318">pdf</a>, <a href="https://arxiv.org/ps/0901.2318">ps</a>, <a href="https://arxiv.org/format/0901.2318">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/10.1086/598968">10.1086/598968 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Close Binary Star Resolved from Occultation by 87 Sylvia </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lin%2C+C">Chi-Long Lin</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+Z">Zhi-Wei Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W+P">W. P. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=King%2C+S">Sun-Kun King</a>, <a href="/search/astro-ph?searchtype=author&query=Lin%2C+H">Hung-Chin Lin</a>, <a href="/search/astro-ph?searchtype=author&query=Bianco%2C+F+B">F. B. Bianco</a>, <a href="/search/astro-ph?searchtype=author&query=Lehner%2C+M+J">M. J. Lehner</a>, <a href="/search/astro-ph?searchtype=author&query=Coehlo%2C+N+K">N. K. Coehlo</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+J+-">J. -H. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Mondal%2C+S">S. Mondal</a>, <a href="/search/astro-ph?searchtype=author&query=Alcock%2C+C">C. Alcock</a>, <a href="/search/astro-ph?searchtype=author&query=Axelrod%2C+T">T. Axelrod</a>, <a href="/search/astro-ph?searchtype=author&query=Byun%2C+Y+-">Y. -I. Byun</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K+H">K. H. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Dave%2C+R">R. Dave</a>, <a href="/search/astro-ph?searchtype=author&query=de+Pater%2C+I">I. de Pater</a>, <a href="/search/astro-ph?searchtype=author&query=Porrata%2C+R">R. Porrata</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D+-">D. -W. Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+T">T. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lissauer%2C+J+J">J. J. Lissauer</a>, <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+S+L">S. L. Marshall</a>, <a href="/search/astro-ph?searchtype=author&query=Rice%2C+J+A">J. A. Rice</a>, <a href="/search/astro-ph?searchtype=author&query=Schwamb%2C+M+E">M. E. Schwamb</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+S+-">S. -Y. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Wen%2C+C+-">C. -Y. Wen</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="0901.2318v1-abstract-short" style="display: inline;"> The star BD+29 1748 was resolved to be a close binary from its occultation by the asteroid 87 Sylvia on 2006 December 18 UT. Four telescopes were used to observe this event at two sites separated by some 80 km apart. Two flux drops were observed at one site, whereas only one flux drop was detected at the other. From the long-term variation of Sylvia, we inferred the probable shape of the shadow… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0901.2318v1-abstract-full').style.display = 'inline'; document.getElementById('0901.2318v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0901.2318v1-abstract-full" style="display: none;"> The star BD+29 1748 was resolved to be a close binary from its occultation by the asteroid 87 Sylvia on 2006 December 18 UT. Four telescopes were used to observe this event at two sites separated by some 80 km apart. Two flux drops were observed at one site, whereas only one flux drop was detected at the other. From the long-term variation of Sylvia, we inferred the probable shape of the shadow during the occultation, and this in turn constrains the binary parameters: the two components of BD+29 1748 have a projected separation of 0.097" to 0.110" on the sky with a position angle 104 deg to 107 deg. The asteroid was clearly resolved with a size scale ranging from 130 to 290 km, as projected onto the occultation direction. No occultation was detected for either of the two known moonlets of 87 Sylvia. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0901.2318v1-abstract-full').style.display = 'none'; document.getElementById('0901.2318v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 January, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2009. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 4 figures, 2 tables; submitted to the PASP</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0901.1285">arXiv:0901.1285</a> <span> [<a href="https://arxiv.org/pdf/0901.1285">pdf</a>, <a href="https://arxiv.org/ps/0901.1285">ps</a>, <a href="https://arxiv.org/format/0901.1285">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1111/j.1365-2966.2009.14615.x">10.1111/j.1365-2966.2009.14615.x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A systematic fitting scheme for caustic-crossing microlensing events </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kains%2C+N">N. Kains</a>, <a href="/search/astro-ph?searchtype=author&query=Cassan%2C+A">A. Cassan</a>, <a href="/search/astro-ph?searchtype=author&query=Horne%2C+K">K. Horne</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">M. D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Dieters%2C+S">S. Dieters</a>, <a href="/search/astro-ph?searchtype=author&query=Fouque%2C+P">P. Fouque</a>, <a href="/search/astro-ph?searchtype=author&query=Greenhill%2C+J">J. Greenhill</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">A. Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Zub%2C+M">M. Zub</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+D+P">D. P. Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Dominik%2C+M">M. Dominik</a>, <a href="/search/astro-ph?searchtype=author&query=Donatowicz%2C+J">J. Donatowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Kubas%2C+D">D. Kubas</a>, <a href="/search/astro-ph?searchtype=author&query=Tsapras%2C+Y">Y. Tsapras</a>, <a href="/search/astro-ph?searchtype=author&query=Anguita%2C+T">T. Anguita</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+V">V. Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Beaulieu%2C+J+-">J. -P. Beaulieu</a>, <a href="/search/astro-ph?searchtype=author&query=Brillant%2C+S">S. Brillant</a>, <a href="/search/astro-ph?searchtype=author&query=Bode%2C+M">M. Bode</a>, <a href="/search/astro-ph?searchtype=author&query=Bramich%2C+D+M">D. M. Bramich</a>, <a href="/search/astro-ph?searchtype=author&query=Burgdorf%2C+M">M. Burgdorf</a>, <a href="/search/astro-ph?searchtype=author&query=Caldwell%2C+J+A+R">J. A. R. Caldwell</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K+H">K. H. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Coutures%2C+C">Ch. Coutures</a>, <a href="/search/astro-ph?searchtype=author&query=Prester%2C+D+D">D. Dominis Prester</a> , et al. (20 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="0901.1285v1-abstract-short" style="display: inline;"> We outline a method for fitting binary-lens caustic-crossing microlensing events based on the alternative model parameterisation proposed and detailed in Cassan (2008). As an illustration of our methodology, we present an analysis of OGLE-2007-BLG-472, a double-peaked Galactic microlensing event with a source crossing the whole caustic structure in less than three days. In order to identify all… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0901.1285v1-abstract-full').style.display = 'inline'; document.getElementById('0901.1285v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0901.1285v1-abstract-full" style="display: none;"> We outline a method for fitting binary-lens caustic-crossing microlensing events based on the alternative model parameterisation proposed and detailed in Cassan (2008). As an illustration of our methodology, we present an analysis of OGLE-2007-BLG-472, a double-peaked Galactic microlensing event with a source crossing the whole caustic structure in less than three days. In order to identify all possible models we conduct an extensive search of the parameter space, followed by a refinement of the parameters with a Markov Chain-Monte Carlo algorithm. We find a number of low-chi2 regions in the parameter space, which lead to several distinct competitive best models. We examine the parameters for each of them, and estimate their physical properties. We find that our fitting strategy locates several minima that are difficult to find with other modelling strategies and is therefore a more appropriate method to fit this type of events. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0901.1285v1-abstract-full').style.display = 'none'; document.getElementById('0901.1285v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 January, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2009. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 11 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/0808.2051">arXiv:0808.2051</a> <span> [<a href="https://arxiv.org/pdf/0808.2051">pdf</a>, <a href="https://arxiv.org/ps/0808.2051">ps</a>, <a href="https://arxiv.org/format/0808.2051">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/592741">10.1086/592741 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First Results From The Taiwanese-American Occultation Survey (TAOS) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+Z+-">Z. -W. Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Bianco%2C+F+B">F. B. Bianco</a>, <a href="/search/astro-ph?searchtype=author&query=Lehner%2C+M+J">M. J. Lehner</a>, <a href="/search/astro-ph?searchtype=author&query=Coehlo%2C+N+K">N. K. Coehlo</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+J+-">J. -H. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Mondal%2C+S">S. Mondal</a>, <a href="/search/astro-ph?searchtype=author&query=Alcock%2C+C">C. Alcock</a>, <a href="/search/astro-ph?searchtype=author&query=Axelrod%2C+T">T. Axelrod</a>, <a href="/search/astro-ph?searchtype=author&query=Byun%2C+Y+-">Y. -I. Byun</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W+-">W. -P. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K+H">K. H. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Dave%2C+R">R. Dave</a>, <a href="/search/astro-ph?searchtype=author&query=de+Pater%2C+I">I. de Pater</a>, <a href="/search/astro-ph?searchtype=author&query=Porrata%2C+R">R. Porrata</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D+-">D. -W. Kim</a>, <a href="/search/astro-ph?searchtype=author&query=King%2C+S+-">S. -K. King</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+T">T. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lin%2C+H+-">H. -C. Lin</a>, <a href="/search/astro-ph?searchtype=author&query=Lissauer%2C+J+J">J. J. Lissauer</a>, <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+S+L">S. L. Marshall</a>, <a href="/search/astro-ph?searchtype=author&query=Protopapas%2C+P">P. Protopapas</a>, <a href="/search/astro-ph?searchtype=author&query=Rice%2C+J+A">J. A. Rice</a>, <a href="/search/astro-ph?searchtype=author&query=Schwamb%2C+M+E">M. E. Schwamb</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+S+-">S. -Y. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Wen%2C+C+-">C. -Y. Wen</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="0808.2051v1-abstract-short" style="display: inline;"> Results from the first two years of data from the Taiwanese-American Occultation Survey (TAOS) are presented. Stars have been monitored photometrically at 4 Hz or 5 Hz to search for occultations by small (~3 km) Kuiper Belt Objects (KBOs). No statistically significant events were found, allowing us to present an upper bound to the size distribution of KBOs with diameters 0.5 km < D < 28 km. </span> <span class="abstract-full has-text-grey-dark mathjax" id="0808.2051v1-abstract-full" style="display: none;"> Results from the first two years of data from the Taiwanese-American Occultation Survey (TAOS) are presented. Stars have been monitored photometrically at 4 Hz or 5 Hz to search for occultations by small (~3 km) Kuiper Belt Objects (KBOs). No statistically significant events were found, allowing us to present an upper bound to the size distribution of KBOs with diameters 0.5 km < D < 28 km. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0808.2051v1-abstract-full').style.display = 'none'; document.getElementById('0808.2051v1-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, 2008; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2008. </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, 5 figure, accepted in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0808.1737">arXiv:0808.1737</a> <span> [<a href="https://arxiv.org/pdf/0808.1737">pdf</a>, <a href="https://arxiv.org/ps/0808.1737">ps</a>, <a href="https://arxiv.org/format/0808.1737">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-6256/136/3/1242">10.1088/0004-6256/136/3/1242 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Properties of Long-Period Variables in the Large Magellanic Cloud from MACHO </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Fraser%2C+O+J">Oliver J. Fraser</a>, <a href="/search/astro-ph?searchtype=author&query=Hawley%2C+S+L">Suzanne L. Hawley</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K+H">Kem H. Cook</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="0808.1737v1-abstract-short" style="display: inline;"> We present a new analysis of the long-period variables in the Large Magellanic Cloud (LMC) from the MACHO Variable Star Catalog. Three-quarters of our sample of evolved, variable stars have periodic light curves. We characterize the stars in our sample using the multiple periods found in their frequency spectra. Additionally, we use single-epoch Two Micron All Sky Survey measurements to construc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0808.1737v1-abstract-full').style.display = 'inline'; document.getElementById('0808.1737v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0808.1737v1-abstract-full" style="display: none;"> We present a new analysis of the long-period variables in the Large Magellanic Cloud (LMC) from the MACHO Variable Star Catalog. Three-quarters of our sample of evolved, variable stars have periodic light curves. We characterize the stars in our sample using the multiple periods found in their frequency spectra. Additionally, we use single-epoch Two Micron All Sky Survey measurements to construct the average infrared light curves for different groups of these stars. Comparison with evolutionary models shows that stars on the red giant branch (RGB) or the early asymptotic giant branch (AGB) often show non-periodic variability, but begin to pulsate with periods on the two shortest period-luminosity sequences (3 & 4) when they brighten to K_s ~ 13. The stars on the thermally pulsing AGB are more likely to pulsate with longer periods that lie on the next two P-L sequences (1 & 2), including the sequence associated with the Miras in the LMC. The Petersen diagram and its variants show that multi-periodic stars on each pair of these sequences (3 & 4, and 1 & 2) typically pulsate with periods associated only with that pair. The periods in these multi-periodic stars become longer and stronger as the star evolves. We further constrain the mechanism behind the long secondary periods (LSPs) seen in half of our sample, and find that there is a close match between the luminosity functions of the LSP stars and all of the stars in our sample, and that these star's pulsation amplitudes are relatively wavelength independent. Although this is characteristic of stellar multiplicity, the large number of these variables is problematic for that explanation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0808.1737v1-abstract-full').style.display = 'none'; document.getElementById('0808.1737v1-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 August, 2008; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2008. </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 AJ; 38 pages, 12 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astron.J.136:1242-1258,2008 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0808.0005">arXiv:0808.0005</a> <span> [<a href="https://arxiv.org/pdf/0808.0005">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> </div> <p class="title is-5 mathjax"> Towards A Census of Earth-mass Exo-planets with Gravitational Microlensing </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Beaulieu%2C+J+P">J. P. Beaulieu</a>, <a href="/search/astro-ph?searchtype=author&query=Kerins%2C+E">E. Kerins</a>, <a href="/search/astro-ph?searchtype=author&query=Mao%2C+S">S. Mao</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+D">D. Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Cassan%2C+A">A. Cassan</a>, <a href="/search/astro-ph?searchtype=author&query=Dieters%2C+S">S. Dieters</a>, <a href="/search/astro-ph?searchtype=author&query=Gaudi%2C+B+S">B. S. Gaudi</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">A. Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+V">V. Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Bender%2C+R">R. Bender</a>, <a href="/search/astro-ph?searchtype=author&query=Brillant%2C+S">S. Brillant</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K">K. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Coutures%2C+C">C. Coutures</a>, <a href="/search/astro-ph?searchtype=author&query=Dominis-Prester%2C+D">D. Dominis-Prester</a>, <a href="/search/astro-ph?searchtype=author&query=Donatowicz%2C+J">J. Donatowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Fouqu%C3%A9%2C+P">P. Fouqu茅</a>, <a href="/search/astro-ph?searchtype=author&query=Grebel%2C+E">E. Grebel</a>, <a href="/search/astro-ph?searchtype=author&query=Greenhill%2C+J">J. Greenhill</a>, <a href="/search/astro-ph?searchtype=author&query=Heyrovsky%2C+D">D. Heyrovsky</a>, <a href="/search/astro-ph?searchtype=author&query=Horne%2C+K">K. Horne</a>, <a href="/search/astro-ph?searchtype=author&query=Kubas%2C+D">D. Kubas</a>, <a href="/search/astro-ph?searchtype=author&query=Marquette%2C+J+B">J. B. Marquette</a>, <a href="/search/astro-ph?searchtype=author&query=Menzies%2C+J">J. Menzies</a>, <a href="/search/astro-ph?searchtype=author&query=Rattenbury%2C+N+J">N. J. Rattenbury</a>, <a href="/search/astro-ph?searchtype=author&query=Ribas%2C+I">I. Ribas</a> , et al. (4 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="0808.0005v1-abstract-short" style="display: inline;"> Thirteen exo-planets have been discovered using the gravitational microlensing technique (out of which 7 have been published). These planets already demonstrate that super-Earths (with mass up to ~10 Earth masses) beyond the snow line are common and multiple planet systems are not rare. In this White Paper we introduce the basic concepts of the gravitational microlensing technique, summarise the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0808.0005v1-abstract-full').style.display = 'inline'; document.getElementById('0808.0005v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0808.0005v1-abstract-full" style="display: none;"> Thirteen exo-planets have been discovered using the gravitational microlensing technique (out of which 7 have been published). These planets already demonstrate that super-Earths (with mass up to ~10 Earth masses) beyond the snow line are common and multiple planet systems are not rare. In this White Paper we introduce the basic concepts of the gravitational microlensing technique, summarise the current mode of discovery and outline future steps towards a complete census of planets including Earth-mass planets. In the near-term (over the next 5 years) we advocate a strategy of automated follow-up with existing and upgraded telescopes which will significantly increase the current planet detection efficiency. In the medium 5-10 year term, we envision an international network of wide-field 2m class telescopes to discover Earth-mass and free-floating exo-planets. In the long (10-15 year) term, we strongly advocate a space microlensing telescope which, when combined with Kepler, will provide a complete census of planets down to Earth mass at almost all separations. Such a survey could be undertaken as a science programme on Euclid, a dark energy probe with a wide-field imager which has been proposed to ESA's Cosmic Vision Programme. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0808.0005v1-abstract-full').style.display = 'none'; document.getElementById('0808.0005v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 July, 2008; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2008. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages. White Paper submission to the ESA Exo-Planet Roadmap Advisory Team. See also "Inferring statistics of planet populations by means of automated microlensing searches" by M. Dominik et al. (arXiv:0808.0004)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0805.4607">arXiv:0805.4607</a> <span> [<a href="https://arxiv.org/pdf/0805.4607">pdf</a>, <a href="https://arxiv.org/ps/0805.4607">ps</a>, <a href="https://arxiv.org/format/0805.4607">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/590427">10.1086/590427 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Scattered-Light Echoes from the Historical Galactic Supernovae Cassiopeia A and Tycho (SN 1572) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rest%2C+A">A. Rest</a>, <a href="/search/astro-ph?searchtype=author&query=Welch%2C+D+L">D. L. Welch</a>, <a href="/search/astro-ph?searchtype=author&query=Suntzeff%2C+N+B">N. B. Suntzeff</a>, <a href="/search/astro-ph?searchtype=author&query=Oaster%2C+L">L. Oaster</a>, <a href="/search/astro-ph?searchtype=author&query=Lanning%2C+H">H. Lanning</a>, <a href="/search/astro-ph?searchtype=author&query=Olsen%2C+K">K. Olsen</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+R+C">R. C. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+A+C">A. C. Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Bergmann%2C+M">M. Bergmann</a>, <a href="/search/astro-ph?searchtype=author&query=Challis%2C+P">P. Challis</a>, <a href="/search/astro-ph?searchtype=author&query=Clocchiatti%2C+A">A. Clocchiatti</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K+H">K. H. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Damke%2C+G">G. Damke</a>, <a href="/search/astro-ph?searchtype=author&query=Garg%2C+A">A. Garg</a>, <a href="/search/astro-ph?searchtype=author&query=Huber%2C+M+E">M. E. Huber</a>, <a href="/search/astro-ph?searchtype=author&query=Matheson%2C+T">T. Matheson</a>, <a href="/search/astro-ph?searchtype=author&query=Minniti%2C+D">D. Minniti</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+J+L">J. L. Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Wood-Vasey%2C+W+M">W. M. Wood-Vasey</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="0805.4607v1-abstract-short" style="display: inline;"> We report the discovery of an extensive system of scattered light echo arclets associated with the recent supernovae in the local neighbourhood of the Milky Way: Tycho (SN 1572) and Cassiopeia A. Existing work suggests that the Tycho SN was a thermonuclear explosion while the Cas A supernova was a core collapse explosion. Precise classifications according to modern nomenclature require spectra o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0805.4607v1-abstract-full').style.display = 'inline'; document.getElementById('0805.4607v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0805.4607v1-abstract-full" style="display: none;"> We report the discovery of an extensive system of scattered light echo arclets associated with the recent supernovae in the local neighbourhood of the Milky Way: Tycho (SN 1572) and Cassiopeia A. Existing work suggests that the Tycho SN was a thermonuclear explosion while the Cas A supernova was a core collapse explosion. Precise classifications according to modern nomenclature require spectra of the outburst light. In the case of ancient SNe, this can only be done with spectroscopy of their light echo, where the discovery of the light echoes from the outburst light is the first step. Adjacent light echo positions suggest that Cas A and Tycho may share common scattering dust structures. If so, it is possible to measure precise distances between historical Galactic supernovae. On-going surveys that alert on the development of bright scattered-light echo features have the potential to reveal detailed spectroscopic information for many recent Galactic supernovae, both directly visible and obscured by dust in the Galactic plane. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0805.4607v1-abstract-full').style.display = 'none'; document.getElementById('0805.4607v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 May, 2008; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2008. </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 color figures, accepted for publication in ApJL</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0805.2366">arXiv:0805.2366</a> <span> [<a href="https://arxiv.org/pdf/0805.2366">pdf</a>, <a href="https://arxiv.org/format/0805.2366">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ab042c">10.3847/1538-4357/ab042c <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> LSST: from Science Drivers to Reference Design and Anticipated Data Products </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ivezi%C4%87%2C+%C5%BD">沤eljko Ivezi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Kahn%2C+S+M">Steven M. Kahn</a>, <a href="/search/astro-ph?searchtype=author&query=Tyson%2C+J+A">J. Anthony Tyson</a>, <a href="/search/astro-ph?searchtype=author&query=Abel%2C+B">Bob Abel</a>, <a href="/search/astro-ph?searchtype=author&query=Acosta%2C+E">Emily Acosta</a>, <a href="/search/astro-ph?searchtype=author&query=Allsman%2C+R">Robyn Allsman</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso%2C+D">David Alonso</a>, <a href="/search/astro-ph?searchtype=author&query=AlSayyad%2C+Y">Yusra AlSayyad</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+S+F">Scott F. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Andrew%2C+J">John Andrew</a>, <a href="/search/astro-ph?searchtype=author&query=Angel%2C+J+R+P">James Roger P. Angel</a>, <a href="/search/astro-ph?searchtype=author&query=Angeli%2C+G+Z">George Z. Angeli</a>, <a href="/search/astro-ph?searchtype=author&query=Ansari%2C+R">Reza Ansari</a>, <a href="/search/astro-ph?searchtype=author&query=Antilogus%2C+P">Pierre Antilogus</a>, <a href="/search/astro-ph?searchtype=author&query=Araujo%2C+C">Constanza Araujo</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+R">Robert Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Arndt%2C+K+T">Kirk T. Arndt</a>, <a href="/search/astro-ph?searchtype=author&query=Astier%2C+P">Pierre Astier</a>, <a href="/search/astro-ph?searchtype=author&query=Aubourg%2C+%C3%89">脡ric Aubourg</a>, <a href="/search/astro-ph?searchtype=author&query=Auza%2C+N">Nicole Auza</a>, <a href="/search/astro-ph?searchtype=author&query=Axelrod%2C+T+S">Tim S. Axelrod</a>, <a href="/search/astro-ph?searchtype=author&query=Bard%2C+D+J">Deborah J. Bard</a>, <a href="/search/astro-ph?searchtype=author&query=Barr%2C+J+D">Jeff D. Barr</a>, <a href="/search/astro-ph?searchtype=author&query=Barrau%2C+A">Aurelian Barrau</a>, <a href="/search/astro-ph?searchtype=author&query=Bartlett%2C+J+G">James G. Bartlett</a> , et al. (288 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="0805.2366v5-abstract-short" style="display: inline;"> (Abridged) We describe here the most ambitious survey currently planned in the optical, the Large Synoptic Survey Telescope (LSST). A vast array of science will be enabled by a single wide-deep-fast sky survey, and LSST will have unique survey capability in the faint time domain. The LSST design is driven by four main science themes: probing dark energy and dark matter, taking an inventory of the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0805.2366v5-abstract-full').style.display = 'inline'; document.getElementById('0805.2366v5-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0805.2366v5-abstract-full" style="display: none;"> (Abridged) We describe here the most ambitious survey currently planned in the optical, the Large Synoptic Survey Telescope (LSST). A vast array of science will be enabled by a single wide-deep-fast sky survey, and LSST will have unique survey capability in the faint time domain. The LSST design is driven by four main science themes: probing dark energy and dark matter, taking an inventory of the Solar System, exploring the transient optical sky, and mapping the Milky Way. LSST will be a wide-field ground-based system sited at Cerro Pach贸n in northern Chile. The telescope will have an 8.4 m (6.5 m effective) primary mirror, a 9.6 deg$^2$ field of view, and a 3.2 Gigapixel camera. The standard observing sequence will consist of pairs of 15-second exposures in a given field, with two such visits in each pointing in a given night. With these repeats, the LSST system is capable of imaging about 10,000 square degrees of sky in a single filter in three nights. The typical 5$蟽$ point-source depth in a single visit in $r$ will be $\sim 24.5$ (AB). The project is in the construction phase and will begin regular survey operations by 2022. The survey area will be contained within 30,000 deg$^2$ with $未<+34.5^\circ$, and will be imaged multiple times in six bands, $ugrizy$, covering the wavelength range 320--1050 nm. About 90\% of the observing time will be devoted to a deep-wide-fast survey mode which will uniformly observe a 18,000 deg$^2$ region about 800 times (summed over all six bands) during the anticipated 10 years of operations, and yield a coadded map to $r\sim27.5$. The remaining 10\% of the observing time will be allocated to projects such as a Very Deep and Fast time domain survey. The goal is to make LSST data products, including a relational database of about 32 trillion observations of 40 billion objects, available to the public and scientists around the world. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0805.2366v5-abstract-full').style.display = 'none'; document.getElementById('0805.2366v5-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 May, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 May, 2008; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2008. </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">57 pages, 32 color figures, version with high-resolution figures available from https://www.lsst.org/overview</span> </p> 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