Subo Dong - Kavli Institute for Astronomy and Astrophysics, Peking University

Subo Dong
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Subo Dong
Kavli Institute for Astronomy and Astrophysics, Peking University

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Solar and Stellar Astrophysics (25)
Earth and Planetary Astrophysics (23)
High Energy Astrophysical Phenomena (16)
Astrophysics of Galaxies (6)
Cosmology and Nongalactic Astrophysics (3)
Instrumentation and Methods for Astrophysics (1)

Publications Authored By Subo Dong

It has recently been discovered that some, if not all, classical novae emit GeV gamma-rays during outburst, but the mechanics of this gamma-ray emission are still not well understood. We present here a comprehensive, multi-wavelength dataset---from radio to X-rays---for the most gamma-ray luminous classical nova to-date, V1324 Sco. Using this dataset, we show that V1324 Sco is a canonical dusty Fe-II type nova, with a bulk ejecta velocity of $1150 \pm 40~\rm km~s^{-1}$ and an ejecta mass of $2. Read More

This manuscript presents information for all supernovae discovered by the All-Sky Automated Survey for SuperNovae (ASAS-SN) during 2015, its second full year of operations. The same information is presented for bright ($m_V\leq17$), spectroscopically confirmed supernovae discovered by other sources in 2015. As with the first ASAS-SN bright supernova catalog, we also present redshifts and near-UV through IR magnitudes for all supernova host galaxies in both samples. Read More

Affiliations: 1Nanjing, 2KIAA-PKU, 3Princeton and Nevada, 4Sydney, 5Utah, 6Royal observatory of Belgium, 7BNU, 8Nanjing, 9NAOC, 10NAOC, 11NAOC, 12Nanjing, 13Nanjing, 14NAOC, 15NIAOT, 16NIAOT, 17NIAOT

The nearly circular (mean eccentricity ~0.06) and coplanar (mean mutual inclination ~3 deg) orbits of the Solar System planets motivated Kant and Laplace to put forth the hypothesis that planets are formed in disks, which has developed into the widely accepted theory of planet formation. Surprisingly, the first several hundred extrasolar planets (mostly Jovian) discovered using the Radial Velocity (RV) technique are commonly on eccentric orbits ( ~ 0. Read More

We report European Very Long Baseline Interferometry Network (EVN) radio continuum observations of ASASSN-14li, one of the best studied tidal disruption events (TDEs) to date. At 1.7 GHz with ~12x6mas resolution, the emission is unresolved. Read More

We present MUSE integral field spectroscopic observations of the host galaxy (PGC 043234) of one of the closest ($z=0.0206$, $D\simeq 90$ Mpc) and best-studied tidal disruption events (TDE), ASASSN-14li. The MUSE integral field data reveal asymmetric and filamentary structures that extend up to $\gtrsim 10$ kpc from the post-starburst host galaxy of ASASSN-14li. Read More

Affiliations: 1Department of Astronomy, The Ohio State University, 2Institute of Astronomy, University of Cambridge, 3Cahill Center for Astrophysics, California Institute of Technology, 4Department of Astronomy, The Ohio State University, 55.6, 6Millennium Institute of Astrophysics, 7Runaway Bay Observatory, 8Department of Astronomy, The Ohio State University, 9Kavli Institute for Astronomy and Astrophysics, Peking University, 10Department of Astronomy, The Ohio State University, 11Department of Astronomy, University of Washington, 12Carnegie Observatories, 13Department of Astronomy, The Ohio State University

We identify a pre-explosion counterpart to the nearby Type IIP supernova ASASSN-16fq (SN 2016cok) in archival Hubble Space Telescope (HST) data. The source appears to be a blend of several stars that prevents obtaining accurate photometry. However, with reasonable assumptions about the stellar temperature and extinction, the progenitor almost certainly had an initial mass M<17Msun, and was most likely in the mass range 8-12Msun. Read More

Outbursts on young stars are usually interpreted as accretion bursts caused by instabilities in the disk or the star-disk connection. However, some protostellar outbursts may not fit into this framework. In this paper, we analyze optical and near-infrared spectra and photometry to characterize the 2015 outburst of the probable young star ASASSN-15qi. Read More

All of the 14 subfields of the Kepler field have been observed at least once with the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST, Xinglong Observatory, China) during the 2012-2014 observation seasons. There are 88,628 reduced spectra with SNR$_g$ (signal-to-noise ratio in g band) $\geq$ 6 after the first round (2012-2014) of observations for the LAMOST-Kepler project (LK-project). By adopting the upgraded version of the LAMOST Stellar Parameter pipeline (LASP), we have determined the atmospheric parameters ($T_{\rm eff}$ , $\log g$, and $\rm [Fe/H]$) and heliocentric radial velocity $v_{\rm rad}$ for 51,406 stars with 61,226 spectra. Read More

We report the discovery and classification of SDSS~J053341.43+001434.1 (SDSS0533), an early-L dwarf first discovered during a powerful $\Delta V < -11$ magnitude flare observed as part of the ASAS-SN survey. Read More

Given its peak luminosity and early-time spectra, ASASSN-15lh was classified as the most luminous supernova (SN) ever discovered (Dong et al. 2016). Here we report a UV rebrightening of ASASSN-15lh observed with Swift during our follow-up campaign. Read More

We present basic statistics for all supernovae discovered by the All-Sky Automated Survey for SuperNovae (ASAS-SN) during its first year-and-a-half of operations, spanning 2013 and 2014. We also present the same information for all other bright ($m_V\leq17$), spectroscopically confirmed supernovae discovered from 2014 May 1 through the end of 2014, providing a comparison to the ASAS-SN sample starting from the point where ASAS-SN became operational in both hemispheres. In addition, we present collected redshifts and near-UV through IR magnitudes, where available, for all host galaxies of the bright supernovae in both samples. Read More

We present ground-based and Swift photometric and spectroscopic observations of the tidal disruption event (TDE) ASASSN-15oi, discovered at the center of 2MASX J20390918-3045201 ($d\simeq216$ Mpc) by the All-Sky Automated Survey for SuperNovae (ASAS-SN). The source peaked at a bolometric luminosity of $L\simeq1.3\times10^{44}$ ergs s$^{-1}$ and radiated a total energy of $E\simeq6. Read More

The double-averaging (DA) approximation is widely employed as the standard technique in studying the secular evolution of the hierarchical three-body system. We show that effects stemmed from the short-timescale oscillations ignored by DA can accumulate over long timescales and lead to significant errors in the long-term evolution of the Lidov-Kozai cycles. In particular, the conditions for having an orbital flip, where the inner orbit switches between prograde and retrograde with respect to the outer orbit and the associated extremely high eccentricities during the switch, can be modified significantly. Read More

We propose that extrasolar asteroid belts can be detected through their gravitational microlensing signatures. Asteroid belt + star lens systems create so-called "pseudo-caustics", regions in the source plane where the magnification exhibits a finite but discontinuous jump. These features allow such systems to generate distinctive signatures in the microlensing light curves for a wide range of belt configurations, with source trajectories as far as tenths of the Einstein ring radius from the centre of the lens. Read More

For all exoplanet candidates, the reliability of a claimed detection needs to be assessed through a careful study of systematic errors in the data to minimize the false positives rate. We present a method to investigate such systematics in microlensing datasets using the microlensing event OGLE-2013-BLG-0446 as a case study. The event was observed from multiple sites around the world and its high magnification (A_{max} \sim 3000) allowed us to investigate the effects of terrestrial and annual parallax. Read More

We report on the mass and distance measurements of two single-lens events from the 2015 \emph{Spitzer} microlensing campaign. With both finite-source effect and microlens parallax measurements, we find that the lens of OGLE-2015-BLG-1268 is very likely a brown dwarf. Assuming that the source star lies behind the same amount of dust as the Bulge red clump, we find the lens is a $45\pm7$ $M_{\rm J}$ brown dwarf at $5. Read More

The nearly continuous light curves with micromagnitude precision provided by the space mission Kepler are revolutionising our view of pulsating stars. They have revealed a vast sea of low-amplitude pulsation modes that were undetectable from Earth. The long time base of Kepler light curves allows an accurate determination of frequencies and amplitudes of pulsation modes needed for in-depth asteroseismic modeling. Read More


We report the detection of a Cold Neptune m_planet=21+/-2MEarth orbiting a 0.38MSol M dwarf lying 2.5-3. Read More

We present Hubble Space Telescope (HST) Wide Field Camera 3 (WFC3) observations of the source and lens stars for planetary microlensing event OGLE-2005-BLG-169, which confirm the relative proper motion prediction due to the planetary light curve signal observed for this event. This (and the companion Keck result) provide the first confirmation of a planetary microlensing signal, for which the deviation was only 2%. The follow-up observations determine the flux of the planetary host star in multiple passbands and remove light curve model ambiguity caused by sparse sampling of part of the light curve. Read More

We report the discovery of ASASSN-15lh (SN 2015L), which we interpret as the most luminous supernova yet found. At redshift z = 0.2326, ASASSN-15lh reached an absolute magnitude of M_{u,AB} = -23. Read More

We present ground-based and Swift photometric and spectroscopic observations of the candidate tidal disruption event (TDE) ASASSN-14li, found at the center of PGC 043234 ($d\simeq90$ Mpc) by the All-Sky Automated Survey for SuperNovae (ASAS-SN). The source had a peak bolometric luminosity of $L\simeq10^{44}$ ergs s$^{-1}$ and a total integrated energy of $E\simeq7\times10^{50}$ ergs radiated over the $\sim6$ months of observations presented. The UV/optical emission of the source is well-fit by a blackbody with roughly constant temperature of $T\sim35,000$ K, while the luminosity declines by roughly a factor of 16 over this time. Read More

We report the discovery of a microlensing exoplanet OGLE-2012-BLG-0563Lb with the planet-star mass ratio ~1 x 10^{-3}. Intensive photometric observations of a high-magnification microlensing event allow us to detect a clear signal of the planet. Although no parallax signal is detected in the light curve, we instead succeed at detecting the flux from the host star in high-resolution JHK'-band images obtained by the Subaru/AO188 and IRCS instruments, allowing us to constrain the absolute physical parameters of the planetary system. Read More

Affiliations: 1Sorbonne Universités, UPMC Univ Paris 6 et CNRS, UMR 7095, Institut d'Astrophysique de Paris, 2Sorbonne Universités, UPMC Univ Paris 6 et CNRS, UMR 7095, Institut d'Astrophysique de Paris, 3University of Canterbury, Dept. of Physics and Astronomy, New Zealand, 4Sorbonne Universités, UPMC Univ Paris 6 et CNRS, UMR 7095, Institut d'Astrophysique de Paris, 5Institute of Natural and Mathematical Sciences, Massey University, Auckland, New Zealand, 6Sorbonne Universités, UPMC Univ Paris 6 et CNRS, UMR 7095, Institut d'Astrophysique de Paris, 7Sorbonne Universités, UPMC Univ Paris 6 et CNRS, UMR 7095, Institut d'Astrophysique de Paris, 8Department of Physics, University of Notre Dame, 9SUPA, School of Physics & Astronomy, North Haugh, University of St Andrews, 10Kavli Institute for Astronomy and Astrophysics, Peking University, 11IRAP, CNRS - Université de Toulouse, 12Department of Astronomy, Ohio State University, 13School of Math and Physics, University of Tasmania, Australia, 14Niels Bohr Institutet, Københavns Universitet, Denmark, 15Space Telescope Science Institute, Baltimore, MD, 16South African Astronomical Observatory, South Africa, 17Department of Earth and Space Science, Osaka University, Japan, 18Qatar Environment and Energy Research Institute, Qatar Foundation, 19Sorbonne Universités, UPMC Univ Paris 6 et CNRS, UMR 7095, Institut d'Astrophysique de Paris, 20Sorbonne Universités, UPMC Univ Paris 6 et CNRS, UMR 7095, Institut d'Astrophysique de Paris, 21Department of Physics, University of Rijeka, Croatia, 22Technical University of Vienna, Department of Computing, 23Department of Astronomy, Ohio State University, 24Department of Physics, Chungbuk National University, Korea, 25SUPA, School of Physics & Astronomy, North Haugh, University of St Andrews, 26SUPA, School of Physics & Astronomy, North Haugh, University of St Andrews, 27Department of Physics and Astronomy, San Francisco State University, 28Korea Astronomy and Space Science Institute, Daejeon, Korea, 29Sorbonne Universités, UPMC Univ Paris 6 et CNRS, UMR 7095, Institut d'Astrophysique de Paris, 30Korea Astronomy and Space Science Institute, Daejeon, Korea, 31University of Canterbury, Dept. of Physics and Astronomy, New Zealand, 32Space Telescope Science Institute, Baltimore, MD, 33Las Cumbres Observatory Global Telescope Network, Goleta, CA, 34Las Cumbres Observatory Global Telescope Network, Goleta, CA, 35Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, 36Perth Observatory, Walnut Road, Bickley, Perth 6076, Australia, 37Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, 38Solar-Terrestrial Environment Laboratory, Nagoya University, Japan, 39Okayama Astrophysical Observatory, National Astronomical Observatory of Japan, 40Solar-Terrestrial Environment Laboratory, Nagoya University, Japan, 41Solar-Terrestrial Environment Laboratory, Nagoya University, Japan, 42Solar-Terrestrial Environment Laboratory, Nagoya University, Japan, 43Solar-Terrestrial Environment Laboratory, Nagoya University, Japan, 44Nagano National College of Technology, Japan, 45Department of Physics, University of Auckland, New Zealand, 46Tokyo Metropolitan College of Aeronautics, Japan, 47School of Chemical and Physical Sciences, Victoria University, Wellington, New Zealand, 48Institute of Information and Mathematical Sciences, Massey University at Albany, Auckland, New Zealand, 49Mt. John University Observatory, Lake Tekapo, New Zealand, 50Department of Physics, University of Auckland, New Zealand, 51Department of Physics, Faculty of Science, Kyoto Sangyo University, Japan

We present the analysis of MOA-2007-BLG-197Lb, the first brown dwarf companion to a Sun-like star detected through gravitational microlensing. The event was alerted and followed-up photometrically by a network of telescopes from the PLANET, MOA, and uFUN collaborations, and observed at high angular resolution using the NaCo instrument at the VLT. From the modelling of the microlensing light curve, we derived the binary lens separation in Einstein radius units (s~1. Read More

Authors: Warren Skidmore, Ian Dell'Antonio, Misato Fukugawa, Aruna Goswami, Lei Hao, David Jewitt, Greg Laughlin, Charles Steidel, Paul Hickson, Luc Simard, Matthias Schöck, Tommaso Treu, Judith Cohen, G. C. Anupama, Mark Dickinson, Fiona Harrison, Tadayuki Kodama, Jessica R. Lu, Bruce Macintosh, Matt Malkan, Shude Mao, Norio Narita, Tomohiko Sekiguchi, Annapurni Subramaniam, Masaomi Tanaka, Feng Tian, Michael A'Hearn, Masayuki Akiyama, Babar Ali, Wako Aoki, Manjari Bagchi, Aaron Barth, Varun Bhalerao, Marusa Bradac, James Bullock, Adam J. Burgasser, Scott Chapman, Ranga-Ram Chary, Masashi Chiba, Michael Cooper, Asantha Cooray, Ian Crossfield, Thayne Currie, Mousumi Das, G. C. Dewangan, Richard de Grijs, Tuan Do, Subo Dong, Jarah Evslin, Taotao Fang, Xuan Fang, Christopher Fassnacht, Leigh Fletcher, Eric Gaidos, Roy Gal, Andrea Ghez, Mauro Giavalisco, Carol A. Grady, Thomas Greathouse, Rupjyoti Gogoi, Puragra Guhathakurta, Luis Ho, Priya Hasan, Gregory J. Herczeg, Mitsuhiko Honda, Masa Imanishi, Hanae Inami, Masanori Iye, Jason Kalirai, U. S. Kamath, Stephen Kane, Nobunari Kashikawa, Mansi Kasliwal, Vishal Kasliwal, Evan Kirby, Quinn M. Konopacky, Sebastien Lepine, Di Li, Jianyang Li, Junjun Liu, Michael C. Liu, Enrigue Lopez-Rodriguez, Jennifer Lotz, Philip Lubin, Lucas Macri, Keiichi Maeda, Franck Marchis, Christian Marois, Alan Marscher, Crystal Martin, Taro Matsuo, Claire Max, Alan McConnachie, Stacy McGough, Carl Melis, Leo Meyer, Michael Mumma, Takayuki Muto, Tohru Nagao, Joan R. Najita, Julio Navarro, Michael Pierce, Jason X. Prochaska, Masamune Oguri, Devendra K. Ojha, Yoshiko K. Okamoto, Glenn Orton, Angel Otarola, Masami Ouchi, Chris Packham, Deborah L. Padgett, Shashi Bhushan Pandey, Catherine Pilachowsky, Klaus M. Pontoppidan, Joel Primack, Shalima Puthiyaveettil, Enrico Ramirez-Ruiz, Naveen Reddy, Michael Rich, Matthew J. Richter, James Schombert, Anjan Ananda Sen, Jianrong Shi, Kartik Sheth, R. Srianand, Jonathan C. Tan, Masayuki Tanaka, Angelle Tanner, Nozomu Tominaga, David Tytler, Vivian U, Lingzhi Wang, Xiaofeng Wang, Yiping Wang, Gillian Wilson, Shelley Wright, Chao Wu, Xufeng Wu, Renxin Xu, Toru Yamada, Bin Yang, Gongbo Zhao, Hongsheng Zhao

The TMT Detailed Science Case describes the transformational science that the Thirty Meter Telescope will enable. Planned to begin science operations in 2024, TMT will open up opportunities for revolutionary discoveries in essentially every field of astronomy, astrophysics and cosmology, seeing much fainter objects much more clearly than existing telescopes. Per this capability, TMT's science agenda fills all of space and time, from nearby comets and asteroids, to exoplanets, to the most distant galaxies, and all the way back to the very first sources of light in the Universe. Read More

The mass of the lenses giving rise to Galactic microlensing events can be constrained by measuring the relative lens-source proper motion and lens flux. The flux of the lens can be separated from that of the source, companions to the source, and unrelated nearby stars with high-resolution images taken when the lens and source are spatially resolved. For typical ground-based adaptive optics (AO) or space-based observations, this requires either inordinately long time baselines or high relative proper motions. Read More

Characterizing a microlensing planet is done from modeling an observed lensing light curve. In this process, it is often confronted that solutions of different lensing parameters result in similar light curves, causing difficulties in uniquely interpreting the lens system, and thus understanding the causes of different types of degeneracy is important. In this work, we show that incomplete coverage of a planetary perturbation can result in degenerate solutions even for events where the planetary signal is detected with a high level of statistical significance. Read More

We examine the luminosity function of white dwarfs (WDs) in the local ``complete'' WD sample ($d<20$ pc) of Holberg et. al. 2008. Read More

We discover clear doubly-peaked line profiles in 3 out of ~20 type Ia supernovae (SNe Ia) with high-quality nebular-phase spectra. The profiles are consistently present in three well-separated Co/Fe emission features. The two peaks are respectively blue-shifted and red-shifted relative to the host galaxies and are separated by ~5000 km/s. Read More

We report the serendipitous discovery of a disk-eclipse system OGLE-LMC-ECL-11893. The eclipse occurs with a period of 468 days, a duration of about 15 days and a deep (up to \Delta I ~1.5), peculiar and asymmetric profile. Read More

We present the first microlensing candidate for a free-floating exoplanet-exomoon system, MOA-2011-BLG-262, with a primary lens mass of M_host ~ 4 Jupiter masses hosting a sub-Earth mass moon. The data are well fit by this exomoon model, but an alternate star+planet model fits the data almost as well. Nevertheless, these results indicate the potential of microlensing to detect exomoons, albeit ones that are different from the giant planet moons in our solar system. Read More

Affiliations: 1KIAA-PKU, 2Utah, 3Princeton, 4Royal observatory of Belgium, 5BNU, 6BNU, NAOC, 7NAOC, 8USTC, 9NIAOT

We use 12000 stars from Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) spectroscopic data to show that the metallicities of Kepler field stars as given in the Kepler Input Catalog (KIC) systematically underestimate both the true metallicity and the dynamic range of the Kepler sample. Specifically, to the first order approximation, we find [Fe/H]_KIC = -0.20 + 0. Read More

We propose a stringent observational test on the formation of warm Jupiters (gas-giant planets with 10 d <~ P <~ 100 d) by high-eccentricity (high-e) migration mechanisms. Unlike hot Jupiters, the majority of observed warm Jupiters have pericenter distances too large to allow efficient tidal dissipation to induce migration. To access the close pericenter required for migration during a Kozai-Lidov cycle, they must be accompanied by a strong enough perturber to overcome the precession caused by General Relativity (GR), placing a strong upper limit on the perturber's separation. Read More

A planetary microlensing signal is generally characterized by a short-term perturbation to the standard single lensing light curve. A subset of binary-source events can produce perturbations that mimic planetary signals, thereby introducing an ambiguity between the planetary and binary-source interpretations. In this paper, we present analysis of the microlensing event MOA-2012-BLG-486, for which the light curve exhibits a short-lived perturbation. Read More

Observations of accretion disks around young brown dwarfs have led to the speculation that they may form planetary systems similar to normal stars. While there have been several detections of planetary-mass objects around brown dwarfs (2MASS 1207-3932 and 2MASS 0441-2301), these companions have relatively large mass ratios and projected separations, suggesting that they formed in a manner analogous to stellar binaries. We present the discovery of a planetary-mass object orbiting a field brown dwarf via gravitational microlensing, OGLE-2012-BLG-0358Lb. Read More

Gravitational microlensing events produced by lenses composed of binary masses are important because they provide a major channel to determine physical parameters of lenses. In this work, we analyze the light curves of two binary-lens events OGLE-2006-BLG-277 and OGLE-2012-BLG-0031 for which the light curves exhibit strong deviations from standard models. From modeling considering various second-order effects, we find that the deviations are mostly explained by the effect of the lens orbital motion. Read More

Type Ia supernovae (SNe Ia), thermonuclear explosions of carbon-oxygen white dwarfs (CO-WDs), are currently the best cosmological "standard candles", but the triggering mechanism of the explosion is unknown. It was recently shown that the rate of head-on collisions of typical field CO-WDs in triple systems may be comparable to the SNe Ia rate. Here we provide evidence supporting a scenario in which the majority of SNe Ia are the result of such head-on collisions of CO-WDs. Read More

Authors: J. -Y. Choi, C. Han, A. Udalski, T. Sumi, B. S. Gaudi, A. Gould, D. P. Bennett, M. Dominik, J. -P. Beaulieu, Y. Tsapras, V. Bozza, F. Abe, I. A. Bond, C. S. Botzler, P. Chote, M. Freeman, A. Fukui, K. Furusawa, Y. Itow, C. H. Ling, K. Masuda, Y. Matsubara, N. Miyake, Y. Muraki, K. Ohnishi, N. J. Rattenbury, To. Saito, D. J. Sullivan, K. Suzuki, W. L. Sweatman, D. Suzuki, S. Takino, P. J. Tristram, K. Wada, P. C. M. Yock, M. K. Szymański, M. Kubiak, G. Pietrzyński, I. Soszyński, J. Skowron, S. Kozłowski, R. Poleski, K. Ulaczyk, Ł. Wyrzykowski, P. Pietrukowicz, L. A. Almeida, D. L. DePoy, Subo Dong, E. Gorbikov, F. Jablonski, C. B. Henderson, K. -H. Hwang, J. Janczak, Y. -K. Jung, S. Kaspi, C. -U. Lee, U. Malamud, D. Maoz, D. McGregor, J. A. Munoz, B. -G. Park, H. Park, R. W. Pogge, Y. Shvartzvald, I. -G. Shin, J. C. Yee, K. A. Alsubai, P. Browne, M. J. Burgdorf, S. Calchi Novati, P. Dodds, X. -S. Fang, F. Finet, M. Glitrup, F. Grundahl, S. -H. Gu, S. Hardis, K. Harpsøe, T. C. Hinse, A. Hornstrup, M. Hundertmark, J. Jessen-Hansen, U. G. Jørgensen, N. Kains, E. Kerins, C. Liebig, M. N. Lund, M. Lundkvist, G. Maier, L. Mancini, M. Mathiasen, M. T. Penny, S. Rahvar, D. Ricci, G. Scarpetta, J. Skottfelt, C. Snodgrass, J. Southworth, J. Surdej, J. Tregloan-Reed, J. Wambsganss, O. Wertz, F. Zimmer, M. D. Albrow, E. Bachelet, V. Batista, S. Brillant, A. Cassan, A. A. Cole, C. Coutures, S. Dieters, D. Dominis Prester, J. Donatowicz, P. Fouqué, J. Greenhill, D. Kubas, J. -B. Marquette, J. W. Menzies, K. C. Sahu, M. Zub, D. M. Bramich, K. Horne, I. A. Steele, R. A. Street

Although many models have been proposed, the physical mechanisms responsible for the formation of low-mass brown dwarfs are poorly understood. The multiplicity properties and minimum mass of the brown-dwarf mass function provide critical empirical diagnostics of these mechanisms. We present the discovery via gravitational microlensing of two very low-mass, very tight binary systems. Read More

An exact relation between the Ni56 mass and the bolometric light curve of a type Ia supernova can be derived as follows, using the following excellent approximations: 1. the emission is powered solely by Ni56-> Co56 ->Fe56; 2. each mass element propagates at a non-relativistic velocity which is constant in time (free coasting); and 3. Read More

We infer the period ($P$) and size ($R_p$) distribution of Kepler transiting planet candidates with $R_p\ge 1 R_{\rm Earth}$ and $P < 250$ days hosted by solar-type stars. The planet detection efficiency is computed by using measured noise and the observed timespans of the light curves for $\sim 120,000$ Kepler target stars. We focus on deriving the shape of planet period and radius distribution functions. Read More

We show that a White Dwarf-White Dwarf (WD-WD) binary with semi-major axis a=1-300 AU, which is orbited by a stellar mass outer perturber with a moderate pericenter r_{p, out} \sim 3-10 x a, has a few percent chance of experiencing a head-on collision within ~5 Gyr. Such a perturber is sufficiently distant to allow the triple system to remain intact for millions of orbits while efficiently exchanging angular momentum with the WD-WD binary. In ~ 5% of the initial orientations, the inner orbit efficiently scans the (equal energy) phase space in the region of zero angular momentum. Read More

Authors: J. C. Yee1, L. -W. Hung2, I. A. Bond3, W. Allen4, L. A. G. Monard5, M. D. Albrow6, P. Fouque7, M. Dominik8, Y. Tsapras9, A. Udalski10, A. Gould11, R. Zellem12, M. Bos13, G. W. Christie14, D. L. DePoy15, Subo Dong16, J. Drummond17, B. S. Gaudi18, E. Gorbikov19, C. Han20, S. Kaspi21, N. Klein22, C. -U. Lee23, D. Maoz24, J. McCormick25, D. Moorhouse26, T. Natusch27, M. Nola28, B. -G. Park29, R. W. Pogge30, D. Polishook31, A. Shporer32, Y. Shvartzvald33, J. Skowron34, G. Thornley35, F. Abe36, D. P. Bennett37, C. S. Botzler38, P. Chote39, M. Freeman40, A. Fukui41, K. Furusawa42, P. Harris43, Y. Itow44, C. H. Ling45, K. Masuda46, Y. Matsubara47, N. Miyake48, K. Ohnishi49, N. J. Rattenbury50, To. Saito51, D. J. Sullivan52, T. Sumi53, D. Suzuki54, W. L. Sweatman55, P. J. Tristram56, K. Wada57, P. C. M. Yock58, M. K. Szymanski59, I. Soszynski60, M. Kubiak61, R. Poleski62, K. Ulaczyk63, G. Pietrzynski64, L. Wyrzykowski65, E. Bachelet66, V. Batista67, T. G. Beatty68, J. -P. Beaulieu69, C. S. Bennett70, R. Bowens-Rubin71, S. Brillant72, J. A. R. Caldwell73, A. Cassan74, A. A. Cole75, E. Corrales76, C. Coutures77, S. Dieters78, D. Dominis Prester79, J. Donatowicz80, J. Greenhill81, C. B. Henderson82, D. Kubas83, J. -B. Marquette84, R. Martin85, J. W. Menzies86, B. Shappee87, A. Williams88, D. Wouters89, J. van Saders90, M. Zub91, R. A. Street92, K. Horne93, D. M. Bramich94, I. A. Steele95, K. A. Alsubai96, V. Bozza97, P. Browne98, M. J. Burgdorf99, S. Calchi Novati100, P. Dodds101, F. Finet102, T. Gerner103, S. Hardis104, K. Harpsoe105, F. V. Hessman106, T. C. Hinse107, M. Hundertmark108, U. G. Jorgensen109, N. Kains110, E. Kerins111, C. Liebig112, L. Mancini113, M. Mathiasen114, M. T. Penny115, S. Proft116, S. Rahvar117, D. Ricci118, K. C. Sahu119, G. Scarpetta120, S. Schafer121, F. Schonebeck122, C. Snodgrass123, J. Southworth124, J. Surdej125, J. Wambsgans126
Affiliations: 1The uFUN Collaboration, 2The uFUN Collaboration, 3The uFUN Collaboration, 4The uFUN Collaboration, 5The uFUN Collaboration, 6The uFUN Collaboration, 7The uFUN Collaboration, 8The uFUN Collaboration, 9The uFUN Collaboration, 10The uFUN Collaboration, 11The uFUN Collaboration, 12The uFUN Collaboration, 13The uFUN Collaboration, 14The uFUN Collaboration, 15The uFUN Collaboration, 16The uFUN Collaboration, 17The uFUN Collaboration, 18The uFUN Collaboration, 19The uFUN Collaboration, 20The uFUN Collaboration, 21The uFUN Collaboration, 22The uFUN Collaboration, 23The uFUN Collaboration, 24The uFUN Collaboration, 25The uFUN Collaboration, 26The uFUN Collaboration, 27The uFUN Collaboration, 28The uFUN Collaboration, 29The uFUN Collaboration, 30The uFUN Collaboration, 31The uFUN Collaboration, 32The uFUN Collaboration, 33The uFUN Collaboration, 34The uFUN Collaboration, 35The uFUN Collaboration, 36The MOA Collaboration, 37The MOA Collaboration, 38The MOA Collaboration, 39The MOA Collaboration, 40The MOA Collaboration, 41The MOA Collaboration, 42The MOA Collaboration, 43The MOA Collaboration, 44The MOA Collaboration, 45The MOA Collaboration, 46The MOA Collaboration, 47The MOA Collaboration, 48The MOA Collaboration, 49The MOA Collaboration, 50The MOA Collaboration, 51The MOA Collaboration, 52The MOA Collaboration, 53The MOA Collaboration, 54The MOA Collaboration, 55The MOA Collaboration, 56The MOA Collaboration, 57The MOA Collaboration, 58The MOA Collaboration, 59The OGLE Collaboration, 60The OGLE Collaboration, 61The OGLE Collaboration, 62The OGLE Collaboration, 63The OGLE Collaboration, 64The OGLE Collaboration, 65The OGLE Collaboration, 66The PLANET Collaboration, 67The PLANET Collaboration, 68The PLANET Collaboration, 69The PLANET Collaboration, 70The PLANET Collaboration, 71The PLANET Collaboration, 72The PLANET Collaboration, 73The PLANET Collaboration, 74The PLANET Collaboration, 75The PLANET Collaboration, 76The PLANET Collaboration, 77The PLANET Collaboration, 78The PLANET Collaboration, 79The PLANET Collaboration, 80The PLANET Collaboration, 81The PLANET Collaboration, 82The PLANET Collaboration, 83The PLANET Collaboration, 84The PLANET Collaboration, 85The PLANET Collaboration, 86The PLANET Collaboration, 87The PLANET Collaboration, 88The PLANET Collaboration, 89The PLANET Collaboration, 90The PLANET Collaboration, 91The PLANET Collaboration, 92The RoboNet Collaboration, 93The RoboNet Collaboration, 94The RoboNet Collaboration, 95The RoboNet Collaboration, 96The MiNDSTEp Consortium, 97The MiNDSTEp Consortium, 98The MiNDSTEp Consortium, 99The MiNDSTEp Consortium, 100The MiNDSTEp Consortium, 101The MiNDSTEp Consortium, 102The MiNDSTEp Consortium, 103The MiNDSTEp Consortium, 104The MiNDSTEp Consortium, 105The MiNDSTEp Consortium, 106The MiNDSTEp Consortium, 107The MiNDSTEp Consortium, 108The MiNDSTEp Consortium, 109The MiNDSTEp Consortium, 110The MiNDSTEp Consortium, 111The MiNDSTEp Consortium, 112The MiNDSTEp Consortium, 113The MiNDSTEp Consortium, 114The MiNDSTEp Consortium, 115The MiNDSTEp Consortium, 116The MiNDSTEp Consortium, 117The MiNDSTEp Consortium, 118The MiNDSTEp Consortium, 119The MiNDSTEp Consortium, 120The MiNDSTEp Consortium, 121The MiNDSTEp Consortium, 122The MiNDSTEp Consortium, 123The MiNDSTEp Consortium, 124The MiNDSTEp Consortium, 125The MiNDSTEp Consortium, 126The MiNDSTEp Consortium

We analyze MOA-2010-BLG-311, a high magnification (A_max>600) microlensing event with complete data coverage over the peak, making it very sensitive to planetary signals. We fit this event with both a point lens and a 2-body lens model and find that the 2-body lens model is a better fit but with only Delta chi^2~80. The preferred mass ratio between the lens star and its companion is $q=10^(-3. Read More

Authors: A. Gould1, J. C. Yee2, I. A. Bond3, A. Udalski4, C. Han5, U. G. Jorgensen6, J. Greenhill7, Y. Tsapras8, M. H. Pinsonneault9, T. Bensby10, W. Allen11, L. A. Almeida12, M. Bos13, G. W. Christie14, D. L. DePoy15, Subo Dong16, B. S. Gaudi17, L. -W. Hung18, F. Jablonski19, C. -U. Lee20, J. McCormick21, D. Moorhouse22, J. A. Munoz23, T. Natusch24, M. Nola25, R. W. Pogge26, J. Skowron27, G. Thornley28, F. Abe29, D. P. Bennett30, C. S. Botzler31, P. Chote32, M. Freeman33, A. Fukui34, K. Furusawa35, P. Harris36, Y. Itow37, C. H. Ling38, K. Masuda39, Y. Matsubara40, N. Miyake41, K. Ohnishi42, N. J. Rattenbury43, To. Saito44, D. J. Sullivan45, T. Sumi46, D. Suzuki47, W. L. Sweatman48, P. J. Tristram49, K. Wada50, P. C. M. Yock51, M. K. Szymanski52, I. Soszynski53, M. Kubiak54, R. Poleski55, K. Ulaczyk56, G. Pietrzynski57, L. Wyrzykowski58, K. A. Alsubai59, V. Bozza60, P. Browne61, M. J. Burgdorf62, S. Calchi Novati63, P. Dodds64, M. Dominik65, F. Finet66, T. Gerner67, S. Hardis68, K. Harpsoe69, F. V. Hessman70, T. C. Hinse71, M. Hundertmark72, N. Kains73, E. Kerins74, C. Liebig75, L. Mancini76, M. Mathiasen77, M. T. Penny78, S. Proft79, S. Rahvar80, D. Ricci81, K. C. Sahu82, G. Scarpetta83, S. Schafer84, F. Schonebeck85, C. Snodgrass86, J. Southworth87, J. Surdej88, J. Wambsganss89, R. A. Street90, K. Horne91, D. M. Bramich92, I. A. Steele93, M. D. Albrow94, E. Bachelet95, V. Batista96, T. G. Beatty97, J. -P. Beaulieu98, C. S. Bennett99, R. Bowens-Rubin100, S. Brillant101, J. A. R. Caldwell102, A. Cassan103, A. A. Cole104, E. Corrales105, C. Coutures106, S. Dieters107, D. Dominis Prester108, J. Donatowicz109, P. Fouque110, C. B. Henderson111, D. Kubas112, J. -B Marquette113, R. Martin114, J. W. Menzies115, B. Shappee116, A. Williams117, J. van Saders118, M. Zub119
Affiliations: 1OSU, 2OSU, 3Massey U., 4Warsaw Obs., 5Chungbuk Nat. U., 6Niels Bohr Inst., 7U. of Tasmania, 8LCOGT, 9OSU, 10Lund Obs., 11The uFUN Collaboration, 12The uFUN Collaboration, 13The uFUN Collaboration, 14The uFUN Collaboration, 15The uFUN Collaboration, 16The uFUN Collaboration, 17The uFUN Collaboration, 18The uFUN Collaboration, 19The uFUN Collaboration, 20The uFUN Collaboration, 21The uFUN Collaboration, 22The uFUN Collaboration, 23The uFUN Collaboration, 24The uFUN Collaboration, 25The uFUN Collaboration, 26The uFUN Collaboration, 27The uFUN Collaboration, 28The uFUN Collaboration, 29The OGLE Collaboration, 30The OGLE Collaboration, 31The OGLE Collaboration, 32The OGLE Collaboration, 33The OGLE Collaboration, 34The OGLE Collaboration, 35The OGLE Collaboration, 36The OGLE Collaboration, 37The OGLE Collaboration, 38The OGLE Collaboration, 39The OGLE Collaboration, 40The OGLE Collaboration, 41The OGLE Collaboration, 42The OGLE Collaboration, 43The OGLE Collaboration, 44The OGLE Collaboration, 45The OGLE Collaboration, 46The OGLE Collaboration, 47The OGLE Collaboration, 48The OGLE Collaboration, 49The OGLE Collaboration, 50The OGLE Collaboration, 51The OGLE Collaboration, 52The OGLE Collaboration, 53The OGLE Collaboration, 54The OGLE Collaboration, 55The OGLE Collaboration, 56The OGLE Collaboration, 57The OGLE Collaboration, 58The OGLE Collaboration, 59The MiNDSTEp Consortium, 60The MiNDSTEp Consortium, 61The MiNDSTEp Consortium, 62The MiNDSTEp Consortium, 63The MiNDSTEp Consortium, 64The MiNDSTEp Consortium, 65The MiNDSTEp Consortium, 66The MiNDSTEp Consortium, 67The MiNDSTEp Consortium, 68The MiNDSTEp Consortium, 69The MiNDSTEp Consortium, 70The MiNDSTEp Consortium, 71The MiNDSTEp Consortium, 72The MiNDSTEp Consortium, 73The MiNDSTEp Consortium, 74The MiNDSTEp Consortium, 75The MiNDSTEp Consortium, 76The MiNDSTEp Consortium, 77The MiNDSTEp Consortium, 78The MiNDSTEp Consortium, 79The MiNDSTEp Consortium, 80The MiNDSTEp Consortium, 81The MiNDSTEp Consortium, 82The MiNDSTEp Consortium, 83The MiNDSTEp Consortium, 84The MiNDSTEp Consortium, 85The MiNDSTEp Consortium, 86The MiNDSTEp Consortium, 87The MiNDSTEp Consortium, 88The MiNDSTEp Consortium, 89The MiNDSTEp Consortium, 90The RoboNet Collaboration, 91The RoboNet Collaboration, 92The RoboNet Collaboration, 93The RoboNet Collaboration, 94The PLANET Collaboration, 95The PLANET Collaboration, 96The PLANET Collaboration, 97The PLANET Collaboration, 98The PLANET Collaboration, 99The PLANET Collaboration, 100The PLANET Collaboration, 101The PLANET Collaboration, 102The PLANET Collaboration, 103The PLANET Collaboration, 104The PLANET Collaboration, 105The PLANET Collaboration, 106The PLANET Collaboration, 107The PLANET Collaboration, 108The PLANET Collaboration, 109The PLANET Collaboration, 110The PLANET Collaboration, 111The PLANET Collaboration, 112The PLANET Collaboration, 113The PLANET Collaboration, 114The PLANET Collaboration, 115The PLANET Collaboration, 116The PLANET Collaboration, 117The PLANET Collaboration, 118The PLANET Collaboration, 119The PLANET Collaboration

The Galactic bulge source MOA-2010-BLG-523S exhibited short-term deviations from a standard microlensing lightcurve near the peak of an Amax ~ 265 high-magnification microlensing event. The deviations originally seemed consistent with expectations for a planetary companion to the principal lens. We combine long-term photometric monitoring with a previously published high-resolution spectrum taken near peak to demonstrate that this is an RS CVn variable, so that planetary microlensing is not required to explain the lightcurve deviations. Read More

We report the discovery of a planetary system from observation of the high-magnification microlensing event OGLE-2012-BLG-0026. The lensing light curve exhibits a complex central perturbation with multiple features. We find that the perturbation was produced by two planets located near the Einstein ring of the planet host star. Read More

A significant fraction of the hot Jupiters with final circularized orbital periods of less than 5 days are thought to form through the channel of high-eccentricity migration. Tidal dissipation at successive periastron passages removes orbital energy of the planet, which has the potential for changes in semi-major axis of a factor of ten to a thousand. In the equilibrium tide approximation we show that, in order for high-eccentricity migration to take place, the relative level of tidal dissipation in Jupiter analogues must be at least 10 times higher than the upper-limit attributed to the Jupiter-Io interaction. Read More

We present the first definitive measurement of the absolute magnitude of RR Lyrae c-type variable stars (RRc) determined purely from statistical parallax. We use a sample of 247 RRc selected from the All Sky Automated Survey (ASAS) for which high-quality light curves, photometry and proper motions are available. We obtain high-resolution echelle spectra for these objects to determine radial velocities and abundances as part of the Carnegie RR Lyrae Survey (CARRS). Read More