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26th Annual Computational Neuroscience Meeting (CNS*2017) of the Organization for Computational Neuroscience Antwerp, Belgium, July 15-20, 2017

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BMC NEUROSCIENCE 2017年第SUPPL 1期18卷 59-59页

作者： [Anonymous] Indiana University Purdue University Indianapolis Indianapolis IN 46032 USA Stark Neurosciences Research Institute Indiana University School of Medicine Indianapolis IN 46032 USA Department of Mathematics East Carolina University Greenville NC 27858 USA Jülich Supercomputing Centre Forschungszentrum Jülich 52425 Jülich Germany Future Systems Swiss National Supercomputing Centre 8092 Zurich Switzerland User Engagement and Support Swiss National Supercomputing Centre 6900 Lugano Switzerland Institut de Neurosciences des Systèmes Aix Marseille Univ 13005 Marseille France Simulation Lab Neuroscience Forschungszentrum Jülich Jülich Germany Department of Experimental Psychology Ghent University 9000 Ghent Belgium Donders Center for Cognitive Neuroimaging Radboud University 6525HR Nijmegen The Netherlands Department of Electrical Computer and Energy Engineering University of Colorado Boulder CO 80309 USA Department of Neurosurgery Johns Hopkins School of Medicine Baltimore MD 21287 USA Department of Neurology Johns Hopkins School of Medicine Baltimore MD 21287 USA Department of Otolaryngology Johns Hopkins School of Medicine Baltimore MD 21287 USA INSERM U968 Paris France Sorbonne Universités UPMC University Paris 06 UMR_S 968 Institut de la Vision Paris France CNRS UMR_7210 Paris France Department of Computer Architecture and Technology University of Granada (CITIC) Granada Spain Sorbonne Universités UPMC Univ Paris 06 INSERM CNRS Institut de la Vision Paris France Department of Adaptive Machine Systems Osaka University Osaka Japan Department of Computer Science University of Cergy-Pontoise Cergy-Pontoise France Department of Physics and Astronomy College of Charleston Charleston SC 29424 USA School of Physics Faculty of Science University of Sydney Sydney NSW 2006 Australia Center of Excellence for Integrative Brain Function Australian Research Council Sydney Australia Max Planck Institute for Human Cognitive and Brain Sciences Saxony Lei

Terahertz emission from the intrinsic Josephson junctions of high-symmetry thermally-managed Bi2Sr2CaCu2O8+δ microstrip antennas

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IOP Conference Series: Materials Science and Engineering 2017年第1期279卷

作者： Richard A. Klemm Andrew E. Davis Qing X. Wang Takashi Yamamoto Daniel P. Cerkoney Candy Reid Maximiliaan L. Koopman Hidetoshi Minami Takanari Kashiwagi Joseph R. Rain Constance M. Doty Michael A. Sedlack Manuel A. Morales Chiharu Watanabe Manabu Tsujimoto Kaveh Delfanazari Kazuo Kadowaki Department of Physics University of Central Florida 4111 Libra Drive Orlando FL 32816-2385 USA Institute for Materials Research Hasselt University Wetenschapspark 1 B-3590 Diepenbeek Belguim Department of Physics and Astronomy Rutgers University 136 Frehlinghuysen Rd. Piscataway NJ 08854 USA Lockheed Martin 5600 Sand Lake Road Orlando FL 32819 USA Graduate School of Pure and Applied Sciences University of Tsukuba 1-1-1 Tennodai Tsukuba Ibaraki 305-8571 Japan Division of Health Science and Technology Harvard Medical School 260 Longwood Ave. Boston MA 02115 USA Department of Physics Cavendish Laboratory University of Cambridge Cambridge CB3 0HE UK

We show for high-symmetry disk, square, or equilateral triangular thin microstrip antennas of any composition respectively obeying C ∞v , C 4v , and C 3v point group symmetries, that the transverse magnetic electromagnetic cavity mode wave functions are restricted in form to those that are one-dimensional representations of those point groups. Plots of the common nodal points of the ten lowest-energy non-radiating two-dimensional representations of each of these three symmetries are presented. For comparison with symmetry-broken disk intrinsic Josephson junction microstrip antennas constructed from the highly anisotropic layered superconductor Bi2Sr2CaCu2O8+δ (BSCCO), we present plots of the ten lowest frequency orthonormal wave functions and of their emission power angular distributions. These results are compared with previous results for square and equilateral triangular thin microstrip antennas.

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An isolated microlens observed from K2, Spitzer and earth

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arXiv 2017年

作者： Zhu, Wei Udalski, A. Huang, C.X. Novati, S. Calchi Sumi, T. Poleski, R. Skowron, J. Mróz, P. Szymanski, M.K. Soszynski, I. Pietrukowicz, P. Koz lowski, S. Ulaczyk, K. Pawlak, M. Beichman, C. Bryden, G. Carey, S. Gaudi, B.S. Gould, A. Henderson, C.B. Shvartzvald, Y. Yee, J.C. Bond, I.A. Bennett, D.P. Suzuki, D. Rattenbury, N.J. Koshimoto, N. Abe, F. Asakura, Y. Barry, R.K. Bhattacharya, A. Donachie, M. Evans, P. Fukui, A. Hirao, Y. Itow, Y. Kawasaki, K. Li, M.C.A. Ling, C.H. Masuda, K. Matsubara, Y. Miyazaki, S. Munakata, H. Muraki, Y. Nagakane, M. Ohnishi, K. Ranc, C. Saito, To. Sharan, A. Sullivan, D.J. Tristram, P.J. Yamada, T. Yonehara, A. Department of Astronomy Ohio State University 140 W. 18th Ave. ColumbusOH43210 United States Canadian Institute for Theoretical Astrophysics University of Toronto 60 St George Street TorontoONM5S 3H8 Canada Warsaw University Observatory Al. Ujazdowskie 4 Warszawa00-478 Poland Department of Physics Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology CambridgeMA02139 United States IPAC Mail Code 100-22 Caltech 1200 E. California Blvd. PasadenaCA91125 United States 84084 Italy Department of Earth and Space Science Graduate School of Science Osaka University 1-1 Machikaneyama Toyonake Osaka560-0043 Japan Department of Physics University of Warwick Gibbert Hill Road CoventryCV4 7AL United Kingdom NASA Exoplanet Science Institute MS 100-22 California Institute of Technology PasadenaCA91125 United States Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Drive PasadenaCA91109 United States Spitzer Science Center MS 220-6 California Institute of Technology PasadenaCA United States Korea Astronomy and Space Science Institute 776 Daedeokdae-ro Yuseong-Gu Daejeon34055 Korea Republic of Max-Planck-Institute for Astronomy Königstuhl 17 Heidelberg69117 Germany NASA Postdoctoral Program Smithsonian Astrophysical Observatory 60 Garden St. CambridgeMA02138 United States Institute for Natural and Mathematical Sciences Massey University North Shore Mail Centre Private Bag 102904 Auckland0745 New Zealand Laboratory for Exoplanets and Stellar Astrophysics NASA/Goddard Space Flight Center GreenbeltMD20771 United States Institute of Space and Astronautical Science Japan Aerospace Exploration Agency 3-1-1 Yoshinodai Chuo Sagamihara Kanagawa252-5210 Japan Department of Physics University of Auckland Private Bag 92019 Auckland New Zealand Institute of Space-Earth Environmental Research Nagoya University Furo-cho Chikusa Nagoya Aichi464-8601 Japan Department of Physics Unive

We present the result of microlensing event MOA-2016-BLG-290, which received observations from the two-wheel Kepler (K2), Spitzer, as well as ground-based observatories. A joint analysis of data from K2 and the ground leads to two degenerate solutions of the lens mass and distance. This degeneracy is effectively broken once the (partial) Spitzer light curve is included. Altogether, the lens is found to be an extremely low-mass star located in the Galactic bulge. MOA-2016-BLG-290 is the first microlensing event for which we have signals from three well-separated (∼ 1 AU) locations. It demonstrates the power of two-satellite microlensing experiment in reducing the ambiguity of lens properties, as pointed out independently by S. Refsdal and A. Gould several decades ago. Copyright © 2017, The Authors. All rights reserved.

关键词： Geometrical optics

Search for extended sources in the galactic plane using 6 years of Fermi-Large area telescope pass 8 data above 10 GeV

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arXiv 2017年

作者： Ackermann, M. Ajello, M. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Bellazzini, R. Bissaldi, E. Bloom, E.D. Bonino, R. Bottacini, E. Brandt, T.J. Bregeon, J. Bruel, P. Buehler, R. Cameron, R.A. Caragiulo, M. Caraveo, P.A. Castro, D. Cavazzuti, E. Cecchi, C. Charles, E. Chekhtman, A. Cheung, C.C. Chiaro, G. Ciprini, S. Cohen, J.M. Costantin, D. Costanza, F. Cutini, S. D’Ammando, F. de Palma, F. Desiante, R. Digel, S.W. Di Lalla, N. Di Mauro, M. Di Venere, L. Favuzzi, C. Fegan, S.J. Ferrara, E.C. Franckowiak, A. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Giglietto, N. Giordano, F. Giroletti, M. Green, D. Grenier, I.A. Grondin, M.-H. Guillemot, L. Guiriec, S. Harding, A.K. Hays, E. Hewitt, J.W. Horan, D. Hou, X. Jóhannesson, G. Kamae, T. Kuss, M. la Mura, G. Larsson, S. Lemoine-Goumard, M. Li, J. Longo, F. Loparco, F. Lubrano, P. Magill, J.D. Maldera, S. Malyshev, D. Manfreda, A. Mazziotta, M.N. Michelson, P.F. Mitthumsiri, W. Mizuno, T. Monzani, M.E. Morselli, A. Moskalenko, I.V. Negro, M. Nuss, E. Ohsugi, T. Omodei, N. Orienti, M. Orlando, E. Ormes, J.F. Paliya, V.S. Paneque, D. Perkins, J.S. Persic, M. Pesce-Rollins, M. Petrosian, V. Piron, F. Porter, T.A. Principe, G. Rainò, S. Rando, R. Razzano, M. Razzaque, S. Reimer, A. Reimer, O. Reposeur, T. Sgrò, C. Simone, D. Siskind, E.J. Spada, F. Spandre, G. Spinelli, P. Suson, D.J. Tak, D. Thayer, J.B. Thompson, D.J. Torres, D.F. Tosti, G. Troja, E. Vianello, G. Wood, K.S. Wood, M. Deutsches Elektronen Synchrotron DESY ZeuthenD-15738 Germany Department of Physics and Astronomy Clemson University Kinard Lab of Physics ClemsonSC29634-0978 United States Università di Pisa Istituto Nazionale di Fisica Nucleare Sezione di Pisa PisaI-56127 Italy Laboratoire AIM CEA-IRFU CNRS Université Paris Diderot Service d’Astrophysique CEA Saclay Gif sur YvetteF-91191 France Istituto Nazionale di Fisica Nucleare Sezione di Trieste TriesteI-34127 Italy Dipartimento di Fisica Università di Trieste TriesteI-34127 Italy Istituto Nazionale di Fisica Nucleare Sezione di Padova PadovaI-35131 Italy Dipartimento di Fisica e Astronomia "G. Galilei" Università di Padova PadovaI-35131 Italy Istituto Nazionale di Fisica Nucleare Sezione di Pisa PisaI-56127 Italy Istituto Nazionale di Fisica Nucleare Sezione di Bari BariI-70126 Italy W. W. Hansen Experimental Physics Laboratory Kavli Institute for Particle Astrophysics and Cosmology Department of Physics SLAC National Accelerator Laboratory Stanford University StanfordCA94305 United States Istituto Nazionale di Fisica Nucleare Sezione di Torino TorinoI-10125 Italy Dipartimento di Fisica Università degli Studi di Torino TorinoI-10125 Italy NASA Goddard Space Flight Center GreenbeltMD20771 United States Laboratoire Univers et Particules de Montpellier Université Montpellier CNRS/IN2P3 MontpellierF-34095 France Laboratoire Leprince-Ringuet École polytechnique CNRS/IN2P3 PalaiseauF-91128 France Dipartimento di Fisica "M. Merlin" dell’Università e del Politecnico di Bari BariI-70126 Italy INAF-Istituto di Astrofisica Spaziale e Fisica Cosmica Milano via E. Bassini 15 MilanoI-20133 Italy Science Data Center RomaI-00133 Italy Istituto Nazionale di Fisica Nucleare Sezione di Perugia PerugiaI-06123 Italy Dipartimento di Fisica Università degli Studi di Perugia PerugiaI-06123 Italy College of Science George Mason University Fairfax VA22030 United States Naval Research Laboratory Washi

The spatial extension of a γ-ray source is an essential ingredient to determine its spectral properties as well as its potential multi-wavelength counterpart. The capability to spatially resolve γ-ray sources is greatly improved by the newly delivered Fermi-Large Area Telescope (LAT) Pass 8 event-level analysis which provides a greater acceptance and an improved point spread function, two crucial factors for the detection of extended sources. Here, we present a complete search for extended sources located within 7◦ from the Galactic plane, using 6 years of Fermi-LAT data above 10 GeV. We find 46 extended sources and provide their morphological and spectral characteristics. This constitutes the first catalog of hard Fermi-LAT extended sources, named the Fermi Galactic Extended Source Catalog, which allows a thorough study of the properties of the Galactic plane in the sub-TeV domain. Copyright © 2017, The Authors. All rights reserved.

关键词： Gamma rays

Cloudless atmospheres for young low-gravity substellar objects

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arXiv 2017年

作者： Tremblin, P. Chabrier, G. Baraffe, I. Liu, Michael C. Magnier, E.A. Lagage, P.-O. De Oliveira, C. Alves Burgasser, A.J. Amundsen, D.S. Drummond, B. Maison de la Simulation CEA CNRS Univ. Paris-Sud UVSQ Université Paris-Saclay Gif-sur-Yvette91191 France Astrophysics Group University of Exeter ExeterEX4 4QL United Kingdom Ecole Normale Supérieure de Lyon CRAL UMR CNRS 5574 Lyon Cedex 0769364 France Institute for Astronomy University of Hawaii 2680 Woodlawn Drive HonoluluHI96822 United States Infrared Telescope Facility University of Hawaii National Aeronautics and Space Administration Science Mission Directorate Planetary Astronomy Program Irfu CEA Université Paris-Saclay Gif-sur YvetteF-9119 France Université Paris Diderot AIM Sorbonne Paris Cité CEA CNRS Gif-sur-YvetteF-91191 France European Space Agency c/o STScI 3700 San Martin Drive BaltimoreMD21218 United States UC San Diego M/C 0424 9500 Gilman Drive La JollaCA92093 United States Department of Applied Physics and Applied Mathematics Columbia University New YorkNY10025 United States NASA Goddard Institute for Space Studies New YorkNY10025 United States

Atmospheric modeling of low-gravity (VL-G) young brown dwarfs remains a challenge. The presence of very thick clouds has been suggested because of their extremely red near-infrared (NIR) spectra, but no cloud models provide a good fit to the data with a radius compatible with evolutionary models for these objects. We show that cloudless atmospheres assuming a temperature gradient reduction caused by fingering convection provides a very good model to match the observed VL-G NIR spectra. The sequence of extremely red colors in the NIR for atmospheres with e_ective temperature from ∼ 2000 K down to ∼ 1200 K is very well reproduced with predicted radii typical of young low-gravity objects. Future observations with NIRSPEC and MIRI on the James Webb Space Telescope (JWST) will provide more constrains in the mid-infrared, helping to confirm/refute whether or not the NIR reddening is caused by fingering convection. We suggest that the presence/absence of clouds will be directly determined by the silicate absorption features that can be observed with MIRI. JWST will therefore be able to better characterize the atmosphere of these hot young brown dwarfs and their low-gravity exoplanet analogues. Copyright © 2017, The Authors. All rights reserved.

关键词： Infrared devices

Blazar spectral variability as explained by a twisting inhomogeneous jet

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arXiv 2017年

作者： Raiteri, C.M. Villata, M. Acosta-Pulido, J.A. Agudo, I. Arkharov, A.A. Bachev, R. Baida, G.V. Benítez, E. Borman, G.A. Boschin, W. Bozhilov, V. Butuzova, M.S. Calcidese, P. Carnerero, M.I. Carosati, D. Casadio, C. Castro-Segura, N. Chen, W.-P. Damljanovic, G. D’Ammando, F. Di Paola, A. Echevarría, J. Efimova, N.V. Ehgamberdiev, Sh A. Espinosa, C. Fuentes, A. Giunta, A. Gómez, J.L. Grishina, T.S. Gurwell, M.A. Hiriart, D. Jermak, H. Jordan, B. Jorstad, S.G. Joshi, M. Kopatskaya, E.N. Kuratov, K. Kurtanidze, O.M. Kurtanidze, S.O. Lähteenmäki, A. Larionov, V.M. Larionova, E.G. Larionova, L.V. Lázaro, C. Lin, C.S. Malmrose, M.P. Marscher, A.P. Matsumoto, K. McBreen, B. Michel, R. Mihov, B. Minev, M. Mirzaqulov, D.O. Mokrushina, A.A. Molina, S.N. Moody, J.W. Morozova, D.A. Nazarov, S.V. Nikolashvili, M.G. Ohlert, J.M. Okhmat, D.N. Ovcharov, E. Pinna, F. Polakis, T.A. Protasio, C. Pursimo, T. Redondo-Lorenzo, F.J. Rizzi, N. Rodriguez-Coira, G. Sadakane, K. Sadun, A.C. Samal, M.R. Savchenko, S.S. Semkov, E. Skiff, B.A. Slavcheva-Mihova, L. Smith, P.S. Steele, I.A. Strigachev, A. Tammi, J. Thum, C. Tornikoski, M. Troitskaya, Yu V. Troitsky, I.S. Vasilyev, A.A. Vince, O. INAF Osservatorio Astrofisico di Torino Pino TorineseI-10025 Italy La Laguna TenerifeE-38200 Spain Departamento de Astrofisica Universidad de La Laguna La Laguna TenerifeE-38205 Spain GranadaE-18080 Spain Pulkovo Observatory St. Petersburg196140 Russia Institute of Astronomy and NAO Bulgarian Academy of Sciences Sofia1784 Bulgaria Crimean Astrophysical Observatory RAS P/O Nauchny298409 Russia Instituto de Astronomía Universidad Nacional Autónoma de México Mexico INAF TNG Fundación Galileo Galilei La PalmaE-38712 Spain Department of Astronomy Faculty of Physics University of Sofia SofiaBG-1164 Bulgaria Osservatorio Astronomico della Regione Autonoma Valle d’Aosta NusI-11020 Italy EPT Observatories Tijarafe La PalmaE-38780 Spain Max-Planck-Institut für Radioastronomie BonnD–53121 Germany School of Physics & Astronomy University of Southampton SouthamptonSO17 1BJ United Kingdom Graduate Institute of Astronomy National Central University Jhongli City Taoyuan County32001 Taiwan Astronomical Observatory Belgrade11060 Serbia Dip. di Fisica e Astronomia Università di Bologna BolognaI-40129 Italy INAF Istituto di Radioastronomia BolognaI-40129 Italy INAF Osservatorio Astronomico di Roma Monte Porzio CatoneI-00040 Italy Ulugh Beg Astronomical Institute Maidanak Observatory Tashkent100052 Uzbekistan Astronomical Institute St. Petersburg State University St. Petersburg198504 Russia Harvard-Smithsonian Center for Astrophysics CambridgeMA02138 United States Astrophysics Research Institute Liverpool John Moores University LiverpoolL3 5RF United Kingdom School of Cosmic Physics Dublin Institute For Advanced Studies Ireland Institute for Astrophysical Research Boston University BostonMA02215 United States NNLOT Al-Farabi Kazakh National University Almaty Kazakhstan Fesenkov Astrophysical Institute Almaty Kazakhstan Abastumani Observatory Mt. Kanobili AbastumaniGA0301 United States Engelhardt Astronomical Observatory Kazan Fe

Blazar emission is dominated by non-thermal radiation from a relativistic jet pointing toward us, therefore undergoing Doppler beaming1. This is responsible for flux enhancement and contraction of the variability time scales, so that most blazars appear as luminous sources characterized by noticeable and fast flux changes at all frequencies. The mechanisms producing their unpredictable variability are debated and include injection, acceleration and cooling of particles2, with possible intervention of shock waves3,4 or turbulence5. Changes in the viewing angle of the emitting knots or jet regions have also been suggested to explain flaring events6,7,8,9,10 or specific properties such as intraday variability11, quasi-periodicities12,13, or the delay of radio flux variations relative to optical changes14. However, such a geometric interpretation has not been universally accepted because alternative explanations based on changes of physical conditions can also work in many cases15,16. Here we report the results of optical-to-radio monitoring of the blazar CTA 102 by the Whole Earth Blazar Telescope Collaboration and show that the observed long-term flux and spectral variability is best explained by an inhomogeneous, curved jet that undergoes orientation changes. We propose that magnetohydrodynamic instabilities17 or rotation of a twisted jet6 cause different jet regions to change their orientation and hence their relative Doppler factors. In particular, the recent extreme optical outburst (six magnitudes) occurred when the corresponding jet emitting region acquired a minimum viewing angle. Copyright © 2017, The Authors. All rights reserved.

关键词： Shock waves

Inside Cover: Dithienyl Acenedithiophenediones as New π-Extended Quinoidal Cores: Synthesis and Properties (Chem. Eur. J. 19/2017)

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Chemistry – A European Journal 2017年第19期23卷 4465-4465页

作者： Dr. Kohsuke Kawabata Prof. Dr. Itaru Osaka Masanori Sawamoto Dr. José L. Zafra Dr. Paula Mayorga Burrezo Prof. Dr. Juan Casado Dr. Kazuo Takimiya Emergent Molecular Function Research Group RIKEN Center for Emergent Matter Science Wako Saitama 351-0198 Japan Current address: Department of Chemical and Environmental Engineering Yale University New Haven Connecticut 06511 USA Current address: Department of Applied Chemistry Graduate School of Engineering Hiroshima University Higashi-Hiroshima 739-8527 Japan Program in Physics and Functional Materials Science Graduate School of Science and Engineering Saitama University Saitama 338-8570 Japan Department of Physical Chemistry Faculty of Science University of Málaga Campus de Teatinos s/n Málaga Spain

Exoplanet biosignatures: A review of remotely detectable signs of life

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arXiv 2017年

作者： Schwieterman, Edward W. Kiang, Nancy Y. Parenteau, Mary N. Harman, Chester E. DasSarma, Shiladitya Fisher, Theresa M. Arney, Giada N. Hartnett, Hilairy E. Reinhard, Christopher T. Olson, Stephanie L. Meadows, Victoria S. Cockell, Charles S. Walker, Sara I. Grenfell, John Lee Hegde, Siddharth Rugheimer, Sarah Hu, Renyu Lyons, Timothy W. Department of Earth Sciences University of California RiversideCA United States NASA Postdoctoral Program Universities Space Research Association ColumbiaMD United States NASA Astrobiology Institute Virtual Planetary Laboratory Team SeattleWA United States NASA Astrobiology Institute Alternative Earths Team RiversideCA United States Blue Marble Space Institute of Science SeattleWA United States NASA Goddard Institute for Space Studies New YorkNY United States NASA Ames Research Center Exobiology Branch Mountain ViewCA United States Department of Applied Physics and Applied Mathematics Columbia University New YorkNY United States Department of Microbiology and Immunology University of Maryland School of Medicine BaltimoreMD United States Institute of Marine and Environmental Technology University System of Maryland BaltimoreMD United States School of Earth and Space Exploration Arizona State University TempeAZ United States Planetary Systems Laboratory NASA Goddard Space Flight Center GreenbeltMD United States School of Molecular Sciences Arizona State University TempeAZ United States School of Earth and Atmospheric Sciences Georgia Institute of Technology AtlantaGA United States Astronomy Department University of Washington SeattleWA United States University of Edinburgh School of Physics and Astronomy Edinburgh United Kingdom UK Centre for Astrobiology Edinburgh United Kingdom Beyond Center for Fundamental Concepts in Science Arizona State University TempeAZ United States ASU-Santa Fe Institute Center for Biosocial Complex Systems Arizona State University TempeAZ United States Berlin Germany Carl Sagan Institute Cornell University IthacaNY United States Cornell Center for Astrophysics and Planetary Science Cornell University IthacaNY United States Department of Earth and Environmental Sciences University of St. Andrews St. Andrews United Kingdom Jet Propulsion Laboratory California Institute of Technology PasadenaCA United St

In the coming years and decades, advanced space- and ground-based observatories will allow an unprecedented opportunity to probe the atmospheres and surfaces of potentially habitable exoplanets for signatures of life. Life on Earth, through its gaseous products and reflectance and scattering properties, has left its fingerprint on the spectrum of our planet. Aided by the universality of the laws of physics and chemistry, we turn to Earth’s biosphere, both in the present and through geologic time, for analog signatures that will aid in the search for life elsewhere. Considering the insights gained from modern and ancient Earth, and the broader array of hypothetical exoplanet possibilities, we have compiled a comprehensive overview of our current understanding of potential exoplanet biosignatures, including gaseous, surface, and temporal biosignatures. We additionally survey biogenic spectral features that are well known in the specialist literature but have not yet been robustly vetted in the context of exoplanet biosignatures. We briefly review advances in assessing biosignature plausibility, including novel methods for determining chemical disequilibrium from remotely obtainable data and assessment tools for determining the minimum biomass required to maintain short-lived biogenic gases as atmospheric signatures. We focus particularly on advances made since the seminal review by Des Marais et al. The purpose of this work is not to propose new biosignature strategies, a goal left to companion articles in this series, but to review the current literature, draw meaningful connections between seemingly disparate areas, and clear the way for a path forward. Copyright © 2017, The Authors. All rights reserved.

关键词： Extrasolar planets

Erratum to: Journal of the Korean Physical Society, Vol. 71, No. 10

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Journal of the Korean Physical Society 2017年第12期71卷 1075-1075页

作者： Shin, Dong Hee Heo, Jin Hyuck Im, Sang Hyuk Lee, Rena Kim, Kyubo Cho, Samju Lim, Sangwook Lee, Suk Shim, Jang Bo Huh, Hyun Do Lee, Sang Hoon Ahn, Sohyun Nobi, Ashadun Lee, Jae Woo Lim, Hyunwoo Lee, Hunwoo Cho, Hyosung Seo, Changwoo Je, Uikyu Park, Chulkyu Kim, Kyuseok Kim, Guna Park, Soyoung Lee, Dongyeon Kang, Seokyoon Lee, Minsik Cao, Jingtai Zhao, Xiaohui Li, Zhaokun Liu, Wei Gu, Haijun Kang, In Ho Na, Moon Kyong Seok, Ogyun Moon, Jeong Hyun Kim, H. W. Kim, Sang Cheol Bahng, Wook Kim, Nam Kyun Park, Him-Chan Yang, Chang Heon Kim, Kyungil Kim, Youngman Lee, Kang Seog Hong, Yoo-Seung Cho, Chun-Hyung Sung, Hyuk-Kee Hyun, June-Won Kim, Gang Bae Lee, Ju Ho Kim, Yeon Jung Hwang, Seungjin Jeong, Jihoon Cho, Seryeyohan Lee, Jongmin Yu, Tae Jun Lee, Kang Il Lee, Geon Joon Park, Gyungsoon Choi, Eun Ha Kim, Dong-Hwan Jeong, Jun-Seok Eom, Su-Keun Lee, Jae-Gil Seo, Kwang-Seok Cha, Ho-Young Ko, Young Joon Kim, Hyun Soo Jung, Jong Hoon Jeong, Inho Song, Hyunwook Lee, B. C. Jang, Hyunchul Kim, Byongju Koo, Sangmo Park, Seran Ko, Dae-Hong Ahn, Kwang Jun Cho, Sungwan Kim, Sang Goon Hong, Kimin Shim, Seung-Bo Jo, Myunglae Cho, Sung Un Park, Yun Daniel Kim, Hee-Cheol Kim, Seok Department of Chemical and Biological Engineering Korea University Seoul Korea Department of radiation Oncology College of Medicine Ewha Womans University Seoul Korea Department of Radiation Oncology Kosin University College of Medicine Busan Korea Department of Radiation Oncology College of Medicine Korea University Seoul Korea Department of Radiation Oncology Inha University Hospital Incheon Korea Department of Radiation Oncology Cheil General Hospital & Women’s Heathcare Center Seoul Korea Department of Radiation Oncology College of Medicine Yonsei University Seoul Korea Department of Computer Science and Telecommunication Engineering Noakhali Science and Technology University Noakhali Bangladesh Department of Physics Inha University Incheon Korea Department of Radiation Convergence Engineering Yonsei University Wonju Korea Department of Radiation Oncology University of Maryland School of Medicine Baltimore USA College of communication Engineering Jilin University Jilin China Changchun Institute of Optics Fine Mechanics and Physics Chinese Academy of Sciences Changchun China College of Geoexploration Science and Technology Jilin University Jilin China Power Semiconductor Research Center Korea Electrotechnology Research Institute (KERI) Changwon Korea Department of Electrical Engineering Kyungnam University Changwon Korea R&D team Maple Semiconductors. Inc. Pohang Korea Rare Isotope Science Project Institute for Basic Science Daejeon Korea Department of Physics Chonnam National University Gwangju Korea School of Electronic and Electrical Engineering Hongik University Seoul Korea Department of Electronic & Electrical Engineering College of Science and Technology Hongik University Sejong Korea Department of Physics Dankook University Cheonan Korea Center for Innovative Engineering Education Dankook University Yongin Korea Department of Advanced Green Energy and Environment Handong Global University Pohang Korea Global Institute of Laser T

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