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  • 1
    Publication Date: 2019
    Print ISSN: 0028-0836
    Electronic ISSN: 1476-4687
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Published by Springer Nature
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  • 2
    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
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  • 3
    Publication Date: 2004-08-31
    Description: Observations of the gravitational microlensing event MOA 2003-BLG-32/OGLE 2003-BLG-219 are presented, for which the peak magnification was over 500, the highest yet reported. Continuous observations around the peak enabled a sensitive search for planets orbiting the lens star. No planets were detected. Planets 1.3 times heavier than Earth were excluded from more than 50% of the projected annular region from approximately 2.3 to 3.6 astronomical units surrounding the lens star, Uranus-mass planets were excluded from 0.9 to 8.7 astronomical units, and planets 1.3 times heavier than Saturn were excluded from 0.2 to 60 astronomical units. These are the largest regions of sensitivity yet achieved in searches for extrasolar planets orbiting any star.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Abe, F -- Bennett, D P -- Bond, I A -- Eguchi, S -- Furuta, Y -- Hearnshaw, J B -- Kamiya, K -- Kilmartin, P M -- Kurata, Y -- Masuda, K -- Matsubara, Y -- Muraki, Y -- Noda, S -- Okajima, K -- Rakich, A -- Rattenbury, N J -- Sako, T -- Sekiguchi, T -- Sullivan, D J -- Sumi, T -- Tristram, P J -- Yanagisawa, T -- Yock, P C M -- Gal-Yam, A -- Lipkin, Y -- Maoz, D -- Ofek, E O -- Udalski, A -- Szewczyk, O -- Zebrun, K -- Soszynski, I -- Szymanski, M K -- Kubiak, M -- Pietrzynski, G -- Wyrzykowski, L -- New York, N.Y. -- Science. 2004 Aug 27;305(5688):1264-6.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Solar Terrestrial Environment Laboratory, Nagoya University, Nagoya 464-01, Japan.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15333833" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
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  • 4
    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〉
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  • 5
    Publication Date: 2014-10-10
    Description: Most ultraluminous X-ray sources have a typical set of properties not seen in Galactic stellar-mass black holes. They have luminosities of more than 3 x 10(39) ergs per second, unusually soft X-ray components (with a typical temperature of less than about 0.3 kiloelectronvolts) and a characteristic downturn in their spectra above about 5 kiloelectronvolts. Such puzzling properties have been interpreted either as evidence of intermediate-mass black holes or as emission from stellar-mass black holes accreting above their Eddington limit, analogous to some Galactic black holes at peak luminosity. Recently, a very soft X-ray spectrum was observed in a rare and transient stellar-mass black hole. Here we report that the X-ray source P13 in the galaxy NGC 7793 is in a binary system with a period of about 64 days and exhibits all three canonical properties of ultraluminous sources. By modelling the strong optical and ultraviolet modulations arising from X-ray heating of the B9Ia donor star, we constrain the black hole mass to be less than 15 solar masses. Our results demonstrate that in P13, soft thermal emission and spectral curvature are indeed signatures of supercritical accretion. By analogy, ultraluminous X-ray sources with similar X-ray spectra and luminosities of up to a few times 10(40) ergs per second can be explained by supercritical accretion onto massive stellar-mass black holes.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Motch, C -- Pakull, M W -- Soria, R -- Grise, F -- Pietrzynski, G -- England -- Nature. 2014 Oct 9;514(7521):198-201. doi: 10.1038/nature13730.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Observatoire astronomique de Strasbourg, Universite de Strasbourg, CNRS, UMR 7550, 11 rue de l'Universite, F-67000 Strasbourg, France. ; International Centre for Radio Astronomy Research, Curtin University, GPO Box U1987, Perth, Western Australia 6845, Australia. ; 1] Observatoire astronomique de Strasbourg, Universite de Strasbourg, CNRS, UMR 7550, 11 rue de l'Universite, F-67000 Strasbourg, France [2] Instituto de Astrofisica de Canarias, Calle Via Lactea, s/n, E-38205 La Laguna, Tenerife, Spain [3] Universidad de La Laguna, Departamento de Astrofisica, E-38206 La Laguna, Tenerife, Spain [4] Department of Physics and Astronomy, University of Iowa, Van Allen Hall, Iowa City, Iowa 52242, USA. ; 1] Universidad de Concepcion, Departamento de Astronomia, Casilla 160-C, Concepcion, Octava Region, Chile [2] Warsaw University Observatory, Aleje Ujazdowskie 4, 00-478 Warszawa, Poland.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/25297432" target="_blank"〉PubMed〈/a〉
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  • 6
    Publication Date: 2015-11-13
    Description: The first stars are predicted to have formed within 200 million years after the Big Bang, initiating the cosmic dawn. A true first star has not yet been discovered, although stars with tiny amounts of elements heavier than helium ('metals') have been found in the outer regions ('halo') of the Milky Way. The first stars and their immediate successors should, however, preferentially be found today in the central regions ('bulges') of galaxies, because they formed in the largest over-densities that grew gravitationally with time. The Milky Way bulge underwent a rapid chemical enrichment during the first 1-2 billion years, leading to a dearth of early, metal-poor stars. Here we report observations of extremely metal-poor stars in the Milky Way bulge, including one star with an iron abundance about 10,000 times lower than the solar value without noticeable carbon enhancement. We confirm that most of the metal-poor bulge stars are on tight orbits around the Galactic Centre, rather than being halo stars passing through the bulge, as expected for stars formed at redshifts greater than 15. Their chemical compositions are in general similar to typical halo stars of the same metallicity although intriguing differences exist, including lower abundances of carbon.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Howes, L M -- Casey, A R -- Asplund, M -- Keller, S C -- Yong, D -- Nataf, D M -- Poleski, R -- Lind, K -- Kobayashi, C -- Owen, C I -- Ness, M -- Bessell, M S -- Da Costa, G S -- Schmidt, B P -- Tisserand, P -- Udalski, A -- Szymanski, M K -- Soszynski, I -- Pietrzynski, G -- Ulaczyk, K -- Wyrzykowski, L -- Pietrukowicz, P -- Skowron, J -- Kozlowski, S -- Mroz, P -- England -- Nature. 2015 Nov 26;527(7579):484-7. doi: 10.1038/nature15747. Epub 2015 Nov 11.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Research School of Astronomy and Astrophysics, Australian National University, Australian Capital Territory 2601, Australia. ; Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK. ; Warsaw University Observatory, Aleje Ujazdowskie 4, 00-478 Warszawa, Poland. ; Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, Ohio 43210, USA. ; Department of Physics and Astronomy, Division of Astronomy and Space Physics, Uppsala University, Box 516, SE-751 20 Uppsala, Sweden. ; School of Physics, Astronomy and Mathematics, Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield AL10 9AB, UK. ; Max-Planck-Institut fur Astronomie, Konigstuhl 17, D-69117 Heidelberg, Germany. ; Sorbonne Universites, UPMC Universite Paris 6 et CNRS, UMR 7095, Institut d'Astrophysique de Paris, 98 bis Boulevard Arago, 75014 Paris, France. ; Universidad de Concepcion, Departamento de Astronomia, Casilla 160-C, Concepcion, Chile. ; Department of Physics, University of Warwick, Gibbet Hill Road, Coventry CV4 7AL, UK.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/26560034" target="_blank"〉PubMed〈/a〉
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  • 7
    Publication Date: 2010-11-26
    Description: Stellar pulsation theory provides a means of determining the masses of pulsating classical Cepheid supergiants-it is the pulsation that causes their luminosity to vary. Such pulsational masses are found to be smaller than the masses derived from stellar evolution theory: this is the Cepheid mass discrepancy problem, for which a solution is missing. An independent, accurate dynamical mass determination for a classical Cepheid variable star (as opposed to type-II Cepheids, low-mass stars with a very different evolutionary history) in a binary system is needed in order to determine which is correct. The accuracy of previous efforts to establish a dynamical Cepheid mass from Galactic single-lined non-eclipsing binaries was typically about 15-30% (refs 6, 7), which is not good enough to resolve the mass discrepancy problem. In spite of many observational efforts, no firm detection of a classical Cepheid in an eclipsing double-lined binary has hitherto been reported. Here we report the discovery of a classical Cepheid in a well detached, double-lined eclipsing binary in the Large Magellanic Cloud. We determine the mass to a precision of 1% and show that it agrees with its pulsation mass, providing strong evidence that pulsation theory correctly and precisely predicts the masses of classical Cepheids.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Pietrzynski, G -- Thompson, I B -- Gieren, W -- Graczyk, D -- Bono, G -- Udalski, A -- Soszynski, I -- Minniti, D -- Pilecki, B -- England -- Nature. 2010 Nov 25;468(7323):542-4. doi: 10.1038/nature09598.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Universidad de Concepcion, Departamento de Astronomia, Casilla 160-C, Concepcion, Chile. pietrzyn@astrouw.edu.pl〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/21107425" target="_blank"〉PubMed〈/a〉
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  • 8
    Publication Date: 2012-04-07
    Description: RR Lyrae pulsating stars have been extensively used as tracers of old stellar populations for the purpose of determining the ages of galaxies, and as tools to measure distances to nearby galaxies. There was accordingly considerable interest when the RR Lyrae star OGLE-BLG-RRLYR-02792 (referred to here as RRLYR-02792) was found to be a member of an eclipsing binary system, because the mass of the pulsator (hitherto constrained only by models) could be unambiguously determined. Here we report that RRLYR-02792 has a mass of 0.26 solar masses M[symbol see text] and therefore cannot be a classical RR Lyrae star. Using models, we find that its properties are best explained by the evolution of a close binary system that started with M[symbol see text] and 0.8M[symbol see text]stars orbiting each other with an initial period of 2.9 days. Mass exchange over 5.4 billion years produced the observed system, which is now in a very short-lived phase where the physical properties of the pulsator happen to place it in the same instability strip of the Hertzsprung-Russell diagram as that occupied by RR Lyrae stars. We estimate that only 0.2 per cent of RR Lyrae stars may be contaminated by systems similar to this one, which implies that distances measured with RR Lyrae stars should not be significantly affected by these binary interlopers.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Pietrzynski, G -- Thompson, I B -- Gieren, W -- Graczyk, D -- Stepien, K -- Bono, G -- Moroni, P G Prada -- Pilecki, B -- Udalski, A -- Soszynski, I -- Preston, G W -- Nardetto, N -- McWilliam, A -- Roederer, I U -- Gorski, M -- Konorski, P -- Storm, J -- England -- Nature. 2012 Apr 4;484(7392):75-7. doi: 10.1038/nature10966.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Departamento de Astronomia, Universidad de Concepcion, Casilla 160-C, Concepcion, Chile. pietrzyn@astrouw.edu.pl〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/22481359" target="_blank"〉PubMed〈/a〉
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  • 9
    Publication Date: 2013-03-08
    Description: In the era of precision cosmology, it is essential to determine the Hubble constant to an accuracy of three per cent or better. At present, its uncertainty is dominated by the uncertainty in the distance to the Large Magellanic Cloud (LMC), which, being our second-closest galaxy, serves as the best anchor point for the cosmic distance scale. Observations of eclipsing binaries offer a unique opportunity to measure stellar parameters and distances precisely and accurately. The eclipsing-binary method was previously applied to the LMC, but the accuracy of the distance results was lessened by the need to model the bright, early-type systems used in those studies. Here we report determinations of the distances to eight long-period, late-type eclipsing systems in the LMC, composed of cool, giant stars. For these systems, we can accurately measure both the linear and the angular sizes of their components and avoid the most important problems related to the hot, early-type systems. The LMC distance that we derive from these systems (49.97 +/- 0.19 (statistical) +/- 1.11 (systematic) kiloparsecs) is accurate to 2.2 per cent and provides a firm base for a 3-per-cent determination of the Hubble constant, with prospects for improvement to 2 per cent in the future.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Pietrzynski, G -- Graczyk, D -- Gieren, W -- Thompson, I B -- Pilecki, B -- Udalski, A -- Soszynski, I -- Kozlowski, S -- Konorski, P -- Suchomska, K -- Bono, G -- Moroni, P G Prada -- Villanova, S -- Nardetto, N -- Bresolin, F -- Kudritzki, R P -- Storm, J -- Gallenne, A -- Smolec, R -- Minniti, D -- Kubiak, M -- Szymanski, M K -- Poleski, R -- Wyrzykowski, L -- Ulaczyk, K -- Pietrukowicz, P -- Gorski, M -- Karczmarek, P -- England -- Nature. 2013 Mar 7;495(7439):76-9. doi: 10.1038/nature11878.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Universidad de Concepcion, Departamento de Astronomia, Casilla 160-C, Concepcion, Chile. pietrzyn@astrouw.edu.pl〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/23467166" target="_blank"〉PubMed〈/a〉
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  • 10
    Publication Date: 2014-07-06
    Description: Using gravitational microlensing, we detected a cold terrestrial planet orbiting one member of a binary star system. The planet has low mass (twice Earth's) and lies projected at ~0.8 astronomical units (AU) from its host star, about the distance between Earth and the Sun. However, the planet's temperature is much lower, 〈60 Kelvin, because the host star is only 0.10 to 0.15 solar masses and therefore more than 400 times less luminous than the Sun. The host itself orbits a slightly more massive companion with projected separation of 10 to 15 AU. This detection is consistent with such systems being very common. Straightforward modification of current microlensing search strategies could increase sensitivity to planets in binary systems. With more detections, such binary-star planetary systems could constrain models of planet formation and evolution.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Gould, A -- Udalski, A -- Shin, I-G -- Porritt, I -- Skowron, J -- Han, C -- Yee, J C -- Kozlowski, S -- Choi, J-Y -- Poleski, R -- Wyrzykowski, L -- Ulaczyk, K -- Pietrukowicz, P -- Mroz, P -- Szymanski, M K -- Kubiak, M -- Soszynski, I -- Pietrzynski, G -- Gaudi, B S -- Christie, G W -- Drummond, J -- McCormick, J -- Natusch, T -- Ngan, H -- Tan, T-G -- Albrow, M -- DePoy, D L -- Hwang, K-H -- Jung, Y K -- Lee, C-U -- Park, H -- Pogge, R W -- Abe, F -- Bennett, D P -- Bond, I A -- Botzler, C S -- Freeman, M -- Fukui, A -- Fukunaga, D -- Itow, Y -- Koshimoto, N -- Larsen, P -- Ling, C H -- Masuda, K -- Matsubara, Y -- Muraki, Y -- Namba, S -- Ohnishi, K -- Philpott, L -- Rattenbury, N J -- Saito, To -- Sullivan, D J -- Sumi, T -- Suzuki, D -- Tristram, P J -- Tsurumi, N -- Wada, K -- Yamai, N -- Yock, P C M -- Yonehara, A -- Shvartzvald, Y -- Maoz, D -- Kaspi, S -- Friedmann, M -- New York, N.Y. -- Science. 2014 Jul 4;345(6192):46-9. doi: 10.1126/science.1251527.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA. ; Warsaw University Observatory, Aleje Ujazdowskie 4, 00-478 Warszawa, Poland. ; Turitea Observatory, Palmerston North, New Zealand. ; Department of Physics, Chungbuk National University, Cheongju 371-763, Republic of Korea. cheongho@astroph.chungbuk.ac.kr. ; Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA. Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA. ; Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA. Warsaw University Observatory, Aleje Ujazdowskie 4, 00-478 Warszawa, Poland. ; Warsaw University Observatory, Aleje Ujazdowskie 4, 00-478 Warszawa, Poland. Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK. ; Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA. Universidad de Concepcion, Departamento de Astronomia, Casilla 160-C, Concepcion, Chile. ; Auckland Observatory, Auckland, New Zealand. ; Possum Observatory, Patutahi, New Zealand. ; Farm Cove Observatory, Centre for Backyard Astrophysics, Pakuranga, Auckland, New Zealand. ; Possum Observatory, Patutahi, New Zealand. Auckland University of Technology, Auckland, New Zealand. ; Perth Exoplanet Survey Telescope, Perth, Australia. ; Department of Physics and Astronomy, University of Canterbury, Private Bag 4800, Christchurch, New Zealand. ; Department of Physics and Astronomy, Texas A&M University, College Station, TX 77843-4242, USA. ; Department of Physics, Chungbuk National University, Cheongju 371-763, Republic of Korea. ; Korea Astronomy and Space Science Institute, Daejeon 305-348, Republic of Korea. ; Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya 464-8601, Japan. ; University of Notre Dame, Department of Physics, 225 Nieuwland Science Hall, Notre Dame, IN 46556-5670, USA. ; Institute of Information and Mathematical Sciences, Massey University, Private Bag 102-904, North Shore Mail Centre, Auckland, New Zealand. ; Department of Physics, University of Auckland, Private Bag 92-019, Auckland 1001, New Zealand. ; Okayama Astrophysical Observatory, National Astronomical Observatory of Japan, Asakuchi, Okayama 719-0232, Japan. ; Department of Earth and Space Science, Osaka University, Osaka 560-0043, Japan. ; Department of Physics, University of Auckland, Private Bag 92-019, Auckland 1001, New Zealand. Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK. ; Nagano National College of Technology, Nagano 381-8550, Japan. ; Department of Earth, Ocean and Atmospheric Sciences, The University of British Columbia, Vancouver, BC V6T 1Z4, Canada. ; Tokyo Metropolitan College of Aeronautics, Tokyo 116-8523, Japan. ; School of Chemical and Physical Sciences, Victoria University, Wellington, New Zealand. ; Mount John University Observatory, Post Office Box 56, Lake Tekapo 8770, New Zealand. ; Department of Physics, Faculty of Science, Kyoto Sangyo University, Kyoto 603-8555, Japan. ; School of Physics and Astronomy, Tel-Aviv University, Tel-Aviv 69978, Israel.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/24994642" target="_blank"〉PubMed〈/a〉
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