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  • 1
    Publication Date: 2008-02-16
    Description: Searches for extrasolar planets have uncovered an astonishing diversity of planetary systems, yet the frequency of solar system analogs remains unknown. The gravitational microlensing planet search method is potentially sensitive to multiple-planet systems containing analogs of all the solar system planets except Mercury. We report the detection of a multiple-planet system with microlensing. We identify two planets with masses of approximately 0.71 and approximately 0.27 times the mass of Jupiter and orbital separations of approximately 2.3 and approximately 4.6 astronomical units orbiting a primary star of mass approximately 0.50 solar mass at a distance of approximately 1.5 kiloparsecs. This system resembles a scaled version of our solar system in that the mass ratio, separation ratio, and equilibrium temperatures of the planets are similar to those of Jupiter and Saturn. These planets could not have been detected with other techniques; their discovery from only six confirmed microlensing planet detections suggests that solar system analogs may be common.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Gaudi, B S -- Bennett, D P -- Udalski, A -- Gould, A -- Christie, G W -- Maoz, D -- Dong, S -- McCormick, J -- Szymanski, M K -- Tristram, P J -- Nikolaev, S -- Paczynski, B -- Kubiak, M -- Pietrzynski, G -- Soszynski, I -- Szewczyk, O -- Ulaczyk, K -- Wyrzykowski, L -- OGLE Collaboration -- Depoy, D L -- Han, C -- Kaspi, S -- Lee, C-U -- Mallia, F -- Natusch, T -- Pogge, R W -- Park, B-G -- MuFUN Collaboration -- Abe, F -- Bond, I A -- Botzler, C S -- Fukui, A -- Hearnshaw, J B -- Itow, Y -- Kamiya, K -- Korpela, A V -- Kilmartin, P M -- Lin, W -- Masuda, K -- Matsubara, Y -- Motomura, M -- Muraki, Y -- Nakamura, S -- Okumura, T -- Ohnishi, K -- Rattenbury, N J -- Sako, T -- Saito, To -- Sato, S -- Skuljan, L -- Sullivan, D J -- Sumi, T -- Sweatman, W L -- Yock, P C M -- MOA Collaboration -- Albrow, M D -- Allan, A -- Beaulieu, J-P -- Burgdorf, M J -- Cook, K H -- Coutures, C -- Dominik, M -- Dieters, S -- Fouque, P -- Greenhill, J -- Horne, K -- Steele, I -- Tsapras, Y -- PLANET and RoboNet Collaborations -- Chaboyer, B -- Crocker, A -- Frank, S -- Macintosh, B -- New York, N.Y. -- Science. 2008 Feb 15;319(5865):927-30. doi: 10.1126/science.1151947.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA. gaudi@astronomy.ohio-state.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/18276883" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 2
    Publication Date: 2012-01-13
    Description: Most known extrasolar planets (exoplanets) have been discovered using the radial velocity or transit 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, 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. These planets are at least as numerous as the stars in the Milky Way. 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(+6)(-9)% of stars host Jupiter-mass planets (0.3-10 M(J), where M(J) = 318 M( plus sign in circle) and M( plus sign in circle) is Earth's mass). Cool Neptunes (10-30 M( plus sign in circle)) and super-Earths (5-10 M( plus sign in circle)) are even more common: their respective abundances per star are 52(+22)(-29)% and 62(+35)(-37)%. We conclude that stars are orbited by planets as a rule, rather than the exception.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Cassan, A -- Kubas, D -- Beaulieu, J-P -- Dominik, M -- Horne, K -- Greenhill, J -- Wambsganss, J -- Menzies, J -- Williams, A -- Jorgensen, U G -- Udalski, A -- Bennett, D P -- Albrow, M D -- Batista, V -- Brillant, S -- Caldwell, J A R -- Cole, A -- Coutures, Ch -- Cook, K H -- Dieters, S -- Prester, D Dominis -- Donatowicz, J -- Fouque, P -- Hill, K -- Kains, N -- Kane, S -- Marquette, J-B -- Martin, R -- Pollard, K R -- Sahu, K C -- Vinter, C -- Warren, D -- Watson, B -- Zub, M -- Sumi, T -- Szymanski, M K -- Kubiak, M -- Poleski, R -- Soszynski, I -- Ulaczyk, K -- Pietrzynski, G -- Wyrzykowski, L -- England -- Nature. 2012 Jan 11;481(7380):167-9. doi: 10.1038/nature10684.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Probing Lensing Anomalies Network (PLANET) Collaboration, Institut d'Astrophysique de Paris, Universite Pierre & Marie Curie, UMR7095 UPMC-CNRS, 98 bis boulevard Arago, 75014 Paris, France. cassan@iap.fr〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/22237108" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0028-0836
    Electronic ISSN: 1476-4687
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
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  • 3
    Publication Date: 1996-05-17
    Description: Candidate pre-main-sequence stars were observed in the bar of the Large Magellanic Cloud during the search for dark matter in the galactic halo. Seven blue stars of apparent visual magnitude 15 to 17 had irregular photometric variations and hydrogen emission lines in their optical spectra, which suggested that these stars are pre-main-sequence stars of about 10 solar masses. These stars are slightly more massive and definitely more luminous than are Herbig AeBe pre-main-sequence stars in our own galaxy. Continued observations of these very young stars from another galaxy, which are probably at the pre-hydrogen-burning stage, should provide important clues about early stages of star formation.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Beaulieu -- Lamers -- Grison -- Julien -- Lanciaux -- Ferlet -- Vidal-Madjar -- Bertin -- Maurice -- Prevot -- Gry -- Guibert -- Moreau -- Tajhmady -- Aubourg -- Bareyre -- de Kat J -- Gros -- Laurent -- Lachieze-Rey -- Lesquoy -- Magneville -- Milsztajn -- Moscoso -- Queinnec -- Renault -- Rich -- Spiro -- Vigroux -- Zylberajch -- Ansari -- Cavalier -- Moniez -- New York, N.Y. -- Science. 1996 May 17;272(5264):995-7.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉The EROS (Experience de Recherche d'Objets Sombres) collaboration: J. P. Beaulieu, P. Grison, R. Julien, C. Lanciaux, R. Ferlet, A. Vidal-Madjar, Institut d'Astrophysique de Paris, 98bis Boulevard, Arago, 75014 Paris, France. H. J. G. L. M. Lamers, Astronomical Institute, Princetonplein 5, NL-3584 CC Utrecht, Netherlands, and SRON Laboratory for Space Research, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. E. Bertin, Institut d'Astrophysique de Paris, 98bis Boulevard, Arago, 75014 Paris, France, and ESO La Silla, casilla 19001, Santiago 19, Chile. E. Maurice and L. Prevot, Observatoire de Marseille, 2 place Le Verrier, 13248 Marseille 04, France. C. Gry, Laboratoire d'Astronomie Spatiale CNRS, Traversee du siphon, les trois lucs, 13120 Marseille, France. J. Guibert, O. Moreau, F. Tajhmady, Centre d'Analyse des Images de l'Institut National des Sciences de l'Univers, CNRS Observatoire de Paris, 61 Avenue de l'Observatoire, 75014 Paris, France. E. Aubourg, P. Bareyre, J. de Kat, M. Gros, B. Laurent, M. Lachieze-Rey, E. Lesquoy, C. Magneville, A. Milsztajn, L. Moscoso, F. Queinnec, C. Renault, J. Rich, M. Spiro, L. Vigroux, S. Zylberajch, CEA, DSM/DAPNIA, Centre d'etudes de Saclay, 91191 Gif-sur-Yvette, France. R. Ansari, F. Cavalier, M. Moniez, Laboratoire de l'Accelerateur Lineaire IN2P3, Centre d'Orsay, 91405 Orsay, France.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/8662586" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 4
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] The 'EROS' (Experience de Recherche d'Objets Sombres) collaboration is searching for microlensing events using the European Southern Observatory at La Silla, Chile4'5. We have two complementary programmes. The first uses 5° x 5° Schmidt plates of the Large Magellanic Cloud ...
    Type of Medium: Electronic Resource
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  • 5
    Publication Date: 2014-11-06
    Description: The Exoplanet Euclid Legacy Survey (ExELS) proposes to determine the frequency of cold exoplanets down to Earth mass from host separations of ~1 au out to the free-floating regime by detecting microlensing events in Galactic bulge. We show that ExELS can also detect large numbers of hot, transiting exoplanets in the same population. The combined microlensing+transit survey would allow the first self-consistent estimate of the relative frequencies of hot and cold sub-stellar companions, reducing biases in comparing ‘near-field’ radial velocity and transiting exoplanets with ‘far-field’ microlensing exoplanets. The age of the bulge and its spread in metallicity further allows ExELS to better constrain both the variation of companion frequency with metallicity and statistically explore the strength of star–planet tides. We conservatively estimate that ExELS will detect ~4100 sub-stellar objects, with sensitivity typically reaching down to Neptune-mass planets. Of these, ~600 will be detectable in both Euclid's VIS (optical) channel and Near Infrared Spectrometer and Photometer (NISP)- H -band imager, with ~90 per cent of detections being hot Jupiters. Likely scenarios predict a range of 2900–7000 for VIS and 400–1600 for H band. Twice as many can be expected in VIS if the cadence can be increased to match the 20-min H -band cadence. The separation of planets from brown dwarfs via Doppler boosting or ellipsoidal variability will be possible in a handful of cases. Radial velocity confirmation should be possible in some cases, using 30 m-class telescopes. We expect secondary eclipses, and reflection and emission from planets to be detectable in up to ~100 systems in both VIS and NISP- H . Transits of ~500 planetary-radius companions will be characterized with two-colour photometry and ~40 with four-colour photometry (VIS, YJH ), and the albedo of (and emission from) a large sample of hot Jupiters in the H band can be explored statistically.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
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  • 6
    Publication Date: 2013-10-18
    Description: Gene families differ in composition, expression, and chromosomal organization between conifers and angiosperms, but little is known regarding nucleotide polymorphism. Using various sequencing strategies, an atlas of 212k high-confidence single nucleotide polymorphisms (SNPs) with a validation rate of more than 92% was developed for the conifer white spruce ( Picea glauca ). Nonsynonymous and synonymous SNPs were annotated over the corresponding 13,498 white spruce genes representative of 2,457 known gene families. Patterns of nucleotide polymorphisms were analyzed by estimating the ratio of nonsynonymous to synonymous numbers of substitutions per site ( A / S ). A general excess of synonymous SNPs was expected and observed. However, the analysis from several perspectives enabled to identify groups of genes harboring an excess of nonsynonymous SNPs, thus potentially under positive selection. Four known gene families harbored such an excess: dehydrins, ankyrin-repeats, AP2/DREB, and leucine-rich repeat. Conifer-specific sequences were also generally associated with the highest A / S ratios. A / S values were also distributed asymmetrically across genes specifically expressed in megagametophytes, roots, or in both, harboring on average an excess of nonsynonymous SNPs. These patterns confirm that the breadth of gene expression is a contributing factor to the evolution of nucleotide polymorphism. The A / S ratios of Medicago truncatula genes were also analyzed: several gene families shared between P. glauca and M. truncatula data sets had similar excess of synonymous or nonsynonymous SNPs. However, a number of families with high A / S ratios were found specific to P. glauca , suggesting cases of divergent evolution at the functional level.
    Electronic ISSN: 1759-6653
    Topics: Biology
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  • 7
    Publication Date: 2013-08-08
    Description: The Euclid mission is the second M-class mission of the ESA Cosmic Vision programme, with the principal science goal of studying dark energy through observations of weak lensing and baryon acoustic oscillations. Euclid is also expected to undertake additional Legacy Science programmes. One such proposal is the Exoplanet Euclid Legacy Survey (ExELS) which will be the first survey able to measure the abundance of exoplanets down to Earth mass for host separations from ~1 au out to the free-floating (unbound) regime. The cold and free-floating exoplanet regimes represent a crucial discovery space for testing planet formation theories. ExELS will use the gravitational microlensing technique and will detect 1000 microlensing events per month over 1.6 deg 2 of the Galactic bulge. We assess how many of these events will have detectable planetary signatures using a detailed multiwavelength microlensing simulator – the Manchester–Besançon microLensing Simulator (MABμLS) – which incorporates the Besançon Galactic model with 3D extinction. MABμLS is the first theoretical simulation of microlensing to treat the effects of point spread function (PSF) blending self-consistently with the underlying Galactic model. We use MABμLS, together with current numerical models for the Euclid PSFs, to explore a number of designs and de-scope options for ExELS, including the exoplanet yield as a function of filter choice and slewing time, and the effect of systematic photometry errors. Using conservative extrapolations of current empirical exoplanet mass functions determined from ground-based microlensing and radial velocity surveys, ExELS can expect to detect a few hundred cold exoplanets around mainly G-, K- and M-type stellar hosts, including ~45 Earth-mass planets and ~6 Mars-mass planets for an observing programme totalling 10 months. ExELS will be capable of measuring the cold exoplanet mass function down to Earth mass or below, with orbital separations ranging from ~1 au out to infinity (i.e. the free-floating regime). Recent ground-based microlensing measurements indicate a significant population of free-floating Jupiters, in which case ExELS will detect hundreds of free-floating planets. ExELS will also be sensitive to hot exoplanets and sub-stellar companions through their transit signatures and this is explored in a companion paper.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
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  • 8
    Publication Date: 2002-11-18
    Print ISSN: 0004-6361
    Electronic ISSN: 1432-0746
    Topics: Physics
    Published by EDP Sciences
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