ALBERT

Description: We simulated the modulation of the interstellar neutral (ISN) He, Ne, and O density and pick-up ion (PUI) production rate and count rate along the Earth's orbit over the solar cycle (SC) from 2002 to 2013 to verify if SC-related effects may modify the inferred ecliptic longitude of the ISN inflow direction. We adopted the classical PUI model with isotropic distribution function and adiabatic cooling, modified by time- and heliolatitude-dependent ionization rates and non-zero injection speed of PUIs. We found that the ionization losses have a noticeable effect on the derivation of the ISN inflow longitude based on the Gaussian fit to the crescent and cone peak locations. We conclude that the non-zero radial velocity of the ISN flow and the energy range of the PUI distribution function that is accumulated are of importance for a precise reproduction of the PUI count rate along the Earth orbit. However, the temporal and latitudinal variations of the ionization in the heliosphere, and particularly their variation on the SC time-scale, may significantly modify the shape of PUI cone and crescent and also their peak positions from year to year and thus bias by a few degrees the derived longitude of the ISN gas inflow direction.

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〉

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〉

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〉

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〉

Description: Neutral gas of the local interstellar medium flows through the inner solar system while being deflected by solar gravity and depleted by ionization. The dominating feature in the energetic neutral atom Interstellar Boundary Explorer (IBEX) all-sky maps at low energies is the hydrogen, helium, and oxygen interstellar gas flow. The He and O flow peaked around 8 February 2009 in accordance with gravitational deflection, whereas H dominated after 26 March 2009, consistent with approximate balance of gravitational attraction by solar radiation pressure. The flow distributions arrive from a few degrees above the ecliptic plane and show the same temperature for He and O. An asymmetric O distribution in ecliptic latitude points to a secondary component from the outer heliosheath.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Mobius, E -- Bochsler, P -- Bzowski, M -- Crew, G B -- Funsten, H O -- Fuselier, S A -- Ghielmetti, A -- Heirtzler, D -- Izmodenov, V V -- Kubiak, M -- Kucharek, H -- Lee, M A -- Leonard, T -- McComas, D J -- Petersen, L -- Saul, L -- Scheer, J A -- Schwadron, N -- Witte, M -- Wurz, P -- New York, N.Y. -- Science. 2009 Nov 13;326(5955):969-71. doi: 10.1126/science.1180971. Epub 2009 Oct 15.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Space Science Center and Department of Physics, University of New Hampshire, Durham, NH 03824, USA. Eberhard.moebius@unh.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/19833917" target="_blank"〉PubMed〈/a〉

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〉

Description: Insects are the most speciose group of animals, but the phylogenetic relationships of many major lineages remain unresolved. We inferred the phylogeny of insects from 1478 protein-coding genes. Phylogenomic analyses of nucleotide and amino acid sequences, with site-specific nucleotide or domain-specific amino acid substitution models, produced statistically robust and congruent results resolving previously controversial phylogenetic relations hips. We dated the origin of insects to the Early Ordovician [~479 million years ago (Ma)], of insect flight to the Early Devonian (~406 Ma), of major extant lineages to the Mississippian (~345 Ma), and the major diversification of holometabolous insects to the Early Cretaceous. Our phylogenomic study provides a comprehensive reliable scaffold for future comparative analyses of evolutionary innovations among insects.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Misof, Bernhard -- Liu, Shanlin -- Meusemann, Karen -- Peters, Ralph S -- Donath, Alexander -- Mayer, Christoph -- Frandsen, Paul B -- Ware, Jessica -- Flouri, Tomas -- Beutel, Rolf G -- Niehuis, Oliver -- Petersen, Malte -- Izquierdo-Carrasco, Fernando -- Wappler, Torsten -- Rust, Jes -- Aberer, Andre J -- Aspock, Ulrike -- Aspock, Horst -- Bartel, Daniela -- Blanke, Alexander -- Berger, Simon -- Bohm, Alexander -- Buckley, Thomas R -- Calcott, Brett -- Chen, Junqing -- Friedrich, Frank -- Fukui, Makiko -- Fujita, Mari -- Greve, Carola -- Grobe, Peter -- Gu, Shengchang -- Huang, Ying -- Jermiin, Lars S -- Kawahara, Akito Y -- Krogmann, Lars -- Kubiak, Martin -- Lanfear, Robert -- Letsch, Harald -- Li, Yiyuan -- Li, Zhenyu -- Li, Jiguang -- Lu, Haorong -- Machida, Ryuichiro -- Mashimo, Yuta -- Kapli, Pashalia -- McKenna, Duane D -- Meng, Guanliang -- Nakagaki, Yasutaka -- Navarrete-Heredia, Jose Luis -- Ott, Michael -- Ou, Yanxiang -- Pass, Gunther -- Podsiadlowski, Lars -- Pohl, Hans -- von Reumont, Bjorn M -- Schutte, Kai -- Sekiya, Kaoru -- Shimizu, Shota -- Slipinski, Adam -- Stamatakis, Alexandros -- Song, Wenhui -- Su, Xu -- Szucsich, Nikolaus U -- Tan, Meihua -- Tan, Xuemei -- Tang, Min -- Tang, Jingbo -- Timelthaler, Gerald -- Tomizuka, Shigekazu -- Trautwein, Michelle -- Tong, Xiaoli -- Uchifune, Toshiki -- Walzl, Manfred G -- Wiegmann, Brian M -- Wilbrandt, Jeanne -- Wipfler, Benjamin -- Wong, Thomas K F -- Wu, Qiong -- Wu, Gengxiong -- Xie, Yinlong -- Yang, Shenzhou -- Yang, Qing -- Yeates, David K -- Yoshizawa, Kazunori -- Zhang, Qing -- Zhang, Rui -- Zhang, Wenwei -- Zhang, Yunhui -- Zhao, Jing -- Zhou, Chengran -- Zhou, Lili -- Ziesmann, Tanja -- Zou, Shijie -- Li, Yingrui -- Xu, Xun -- Zhang, Yong -- Yang, Huanming -- Wang, Jian -- Wang, Jun -- Kjer, Karl M -- Zhou, Xin -- New York, N.Y. -- Science. 2014 Nov 7;346(6210):763-7. doi: 10.1126/science.1257570. Epub 2014 Nov 6.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Zoologisches Forschungsmuseum Alexander Koenig (ZFMK)/Zentrum fur Molekulare Biodiversitatsforschung (ZMB), Bonn, Germany. xinzhou@genomics.cn b.misof.zfmk@uni-bonn.de kjer@aesop.rutgers.edu wangj@genomics.cn. ; China National GeneBank, BGI-Shenzhen, China. BGI-Shenzhen, China. ; Zoologisches Forschungsmuseum Alexander Koenig (ZFMK)/Zentrum fur Molekulare Biodiversitatsforschung (ZMB), Bonn, Germany. Australian National Insect Collection, Commonwealth Scientific and Industrial Research Organization (Australia) (CSIRO), National Research Collections Australia, Canberra, ACT, Australia. ; Abteilung Arthropoda, Zoologisches Forschungsmuseum Alexander Koenig (ZFMK), Bonn, Germany. ; Zoologisches Forschungsmuseum Alexander Koenig (ZFMK)/Zentrum fur Molekulare Biodiversitatsforschung (ZMB), Bonn, Germany. ; Department of Entomology, Rutgers University, New Brunswick, NJ 08854, USA. ; Department of Biological Sciences, Rutgers University, Newark, NJ 08854, USA. ; Scientific Computing, Heidelberg Institute for Theoretical Studies (HITS), Heidelberg, Germany. ; Institut fur Spezielle Zoologie und Evolutionsbiologie mit Phyletischem Museum Jena, FSU Jena, Germany. ; Steinmann-Institut, Bereich Palaontologie, Universitat Bonn, Germany. ; 2. Zoologische Abteilung (Insekten), Naturhistorisches Museum Wien, Vienna, Austria. Department of Integrative Zoology, Universitat Wien, Vienna, Austria. ; Institut fur Spezifische Prophylaxe und Tropenmedizin, Medizinische Parasitologie, Medizinische Universitat Wien (MUW), Vienna, Austria. ; Department of Integrative Zoology, Universitat Wien, Vienna, Austria. ; Zoologisches Forschungsmuseum Alexander Koenig (ZFMK)/Zentrum fur Molekulare Biodiversitatsforschung (ZMB), Bonn, Germany. Sugadaira Montane Research Center/Hexapod Comparative Embryology Laboratory, University of Tsukuba, Japan. ; Manaaki Whenua Landcare Research, Auckland, New Zealand. ; Center for Advanced Modeling, Emergency Medicine Department, Johns Hopkins University, Baltimore, MD 21209, USA. ; BGI-Shenzhen, China. ; Biozentrum Grindel und Zoologisches Museum, Universitat Hamburg, Hamburg, Germany. ; Evolutionary Morphology Laboratory, Graduate School of Science and Engineering, Ehime University, Japan. ; Sugadaira Montane Research Center/Hexapod Comparative Embryology Laboratory, University of Tsukuba, Japan. ; Land and Water Flagship, CSIRO, Canberra, ACT, Australia. ; Florida Museum of Natural History, University of Florida, Gainesville, FL 32611, USA. ; Entomology, Staatliches Museum fur Naturkunde Stuttgart (SMNS), Germany. ; Ecology Evolution and Genetics, Research School of Biology, Australian National University, Canberra, ACT, Australia. National Evolutionary Synthesis Center, Durham, NC 27705, USA. Department of Biological Sciences, Macquarie University, Sydney, Australia. ; Department fur Botanik und Biodiversitatsforschung, Universitat Wien, Vienna, Austria. ; Scientific Computing, Heidelberg Institute for Theoretical Studies (HITS), Heidelberg, Germany. Natural History Museum of Crete, University of Crete, Post Office Box 2208, Gr-71409, Iraklio, and Biology Department, University of Crete, Iraklio, Crete, Greece. ; Department of Biological Sciences and Feinstone Center for Genomic Research, University of Memphis, Memphis, TN 38152, USA. ; Centro Universitario de Ciencias Biologicas y Agropecuarias, Centro de Estudios en Zoologia, Universidad de Guadalajara, Zapopan, Jalisco, Mexico. ; Leibniz Supercomputing Centre of the Bavarian Academy of Sciences and Humanities, Garching, Germany. ; Institute of Evolutionary Biology and Ecology, Zoology and Evolutionary Biology, University of Bonn, Bonn, Germany. ; Department of Life Sciences, The Natural History Museum London, London, UK. ; Abteilung Entomologie, Biozentrum Grindel und Zoologisches Museum, Universitat Hamburg, Hamburg, Germany. ; Australian National Insect Collection, Commonwealth Scientific and Industrial Research Organization (Australia) (CSIRO), National Research Collections Australia, Canberra, ACT, Australia. ; Scientific Computing, Heidelberg Institute for Theoretical Studies (HITS), Heidelberg, Germany. Fakultat fur Informatik, Karlsruher Institut fur Technologie, Karlsruhe, Germany. ; California Academy of Sciences, San Francisco, CA 94118, USA. ; Department of Entomology, College of Natural Resources and Environment, South China Agricultural University, China. ; Sugadaira Montane Research Center/Hexapod Comparative Embryology Laboratory, University of Tsukuba, Japan. Yokosuka City Museum, Yokosuka, Kanagawa, Japan. ; Department of Entomology, North Carolina State University, Raleigh, NC 27695, USA. ; Systematic Entomology, Hokkaido University, Sapporo, Japan. ; BGI-Shenzhen, China. Department of Biology, University of Copenhagen, Copenhagen, Denmark. Princess Al Jawhara Center of Excellence in the Research of Hereditary Disorders, King Abdulaziz University, Jeddah, Saudi Arabia. Macau University of Science and Technology, Avenida Wai Long, Taipa, Macau, China. Department of Medicine, University of Hong Kong, Hong Kong. xinzhou@genomics.cn b.misof.zfmk@uni-bonn.de kjer@aesop.rutgers.edu wangj@genomics.cn. ; Department of Ecology, Evolution, and Natural Resources, Rutgers University, New Brunswick, NJ 08854, USA. xinzhou@genomics.cn b.misof.zfmk@uni-bonn.de kjer@aesop.rutgers.edu wangj@genomics.cn. ; China National GeneBank, BGI-Shenzhen, China. BGI-Shenzhen, China. xinzhou@genomics.cn b.misof.zfmk@uni-bonn.de kjer@aesop.rutgers.edu wangj@genomics.cn.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/25378627" target="_blank"〉PubMed〈/a〉

Description: The effective design of an artificial photosynthetic system entails the optimization of several important interactions. Herein we report stopped-flow UV-visible (UV-vis) spectroscopy, X-ray crystallographic, density functional theory (DFT), and electrochemical kinetic studies of the Re(bipy-tBu)(CO)3(L) catalyst for the reduction of CO2 to CO. A remarkable selectivity for CO2 over H+...