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Atomic Mass Evaluation: the Mass Tables
G. Audi,M. Wang,A. H. Wapstra,B. Pfeiffer,F. G. Kondev 한국물리학회 2011 THE JOURNAL OF THE KOREAN PHYSICAL SOCIETY Vol.59 No.23
The advent of the ``AME-Future" project a year and a half ago rendered the realization of a new mass table possible in the very near future: the Ame2013 mass table. A large number of the new experimental data obtained from different laboratories have already been analyzed. They exhibit important changes in the mass surface. Most of these changes lift the mass surface to higher masses (reduced binding energies). The rise can be explained by previously under-estimated Q_β data of exotic species due to missed levels. Some consequences of this change are expected in calculations using the nuclear masses as one of their ingredients. We will discuss here the expected impact on the nucleo-synthesis r-process path in astrophysics.
OPTIMAL SURVEY STRATEGIES AND PREDICTED PLANET YIELDS FOR THE KOREAN MICROLENSING TELESCOPE NETWORK
Henderson, Calen B.,Gaudi, B. Scott,Han, Cheongho,Skowron, Jan,Penny, Matthew T.,Nataf, David,Gould, Andrew P. IOP Publishing 2014 The Astrophysical journal Vol.794 No.1
<P>The Korean Microlensing Telescope Network (KMTNet) will consist of three 1.6 m telescopes each with a 4 deg(2) field of view (FoV) and will be dedicated to monitoring the Galactic Bulge to detect exoplanets via gravitational microlensing. KMTNet's combination of aperture size, FoV, cadence, and longitudinal coverage will provide a unique opportunity to probe exoplanet demographics in an unbiased way. Here we present simulations that optimize the observing strategy for and predict the planetary yields of KMTNet. We find preferences for four target fields located in the central Bulge and an exposure time of t(exp) = 120 s, leading to the detection of similar to 2200 microlensing events per year. We estimate the planet detection rates for planets with mass and separation across the ranges 0.1 <= M-p/M-circle plus <= 1000 and 0.4 <= a/AU <= 16, respectively. Normalizing these rates to the cool-planet mass function of Cassan et al., we predict KMTNet will be approximately uniformly sensitive to planets with mass 5 <= M-p/M-circle plus <= 1000 and will detect similar to 20 planets per year per dex in mass across that range. For lower-mass planets with mass 0.1 <= M-p/M-circle plus < 5, we predict KMTNet will detect similar to 10 planets per year. We also compute the yields KMTNet will obtain for free-floating planets (FFPs) and predict KMTNet will detect similar to 1 Earth-mass FFP per year, assuming an underlying population of one such planet per star in the Galaxy. Lastly, we investigate the dependence of these detection rates on the number of observatories, the photometric precision limit, and optimistic assumptions regarding seeing, throughput, and flux measurement uncertainties.</P>
MICROLENSING EVENT MOA-2007-BLG-400: EXHUMING THE BURIED SIGNATURE OF A COOL, JOVIAN-MASS PLANET
Dong, Subo,Bond, I. A.,Gould, A.,Kozłowski, Szymon,Miyake, N.,Gaudi, B. S.,Bennett, D. P.,Abe, F.,Gilmore, A. C.,Fukui, A.,Furusawa, K.,Hearnshaw, J. B.,Itow, Y.,Kamiya, K.,Kilmartin, P. M.,Korpela, A IOP Publishing 2009 The Astrophysical journal Vol.698 No.2
OGLE-2005-BLG-071Lb, THE MOST MASSIVE M DWARF PLANETARY COMPANION?
Dong, Subo,Gould, Andrew,Udalski, Andrzej,Anderson, Jay,Christie, G. W.,Gaudi, B. S.,Jaroszyń,ski, M.,Kubiak, M.,Szymań,ski, M. K.,Pietrzyń,ski, G.,Soszyń,ski, I.,Szewczyk, O.,Ulac IOP Publishing 2009 The Astrophysical journal Vol.695 No.2
Han, C.,Jung, Y. K.,Udalski, A.,Sumi, T.,Gaudi, B. S.,Gould, A.,Bennett, D. P.,Tsapras, Y.,Szymań,ski, M. K.,Kubiak, M.,Pietrzyń,ski, G.,Soszyń,ski, I.,Skowron, J.,Kozłowski, S.,Poleski IOP Publishing 2013 The Astrophysical journal Vol.778 No.1
<P>Observations of accretion disks around young brown dwarfs (BDs) 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 BDs (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 BD via gravitational microlensing, OGLE-2012-BLG-0358Lb. The system is a low secondary/primary mass ratio (0.080 +/- 0.001), relatively tightly separated (similar to 0.87 AU) binary composed of a planetary-mass object with 1.9 +/- 0.2 Jupiter masses orbiting a BD with a mass 0.022M(circle dot). The relatively small mass ratio and separation suggest that the companion may have formed in a protoplanetary disk around the BD host in a manner analogous to planets.</P>
MASSES AND ORBITAL CONSTRAINTS FOR THE OGLE-2006-BLG-109Lb,c JUPITER/SATURN ANALOG PLANETARY SYSTEM
Bennett, D. P.,Rhie, S. H.,Nikolaev, S.,Gaudi, B. S.,Udalski, A.,Gould, A.,Christie, G. W.,Maoz, D.,Dong, S.,McCormick, J.,Szymań,ski, M. K.,Tristram, P. J.,Macintosh, B.,Cook, K. H.,Kubiak, M.,P IOP Publishing 2010 The Astrophysical journal Vol.713 No.2
<P>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(-0.04)(+0.05) M(circle dot), M(b) = 231 +/- 19 M(circle plus), and M(c) = 86 +/- 7 M(circle plus). 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 epsilon = 0.15(-0.10) (+0.17) and an orbital inclination of i = 64 degrees(+ 4 degrees)(-7 degrees) The 95% confidence level lower limit on the inclination of i > 49 degrees implies that this planetary system can be detected and studied via radial velocity measurements using a telescope of greater than or similar to 30 m aperture.</P>