Planck 2015 results - XIII. Cosmological parameters
Peter A. R. Ade,Nabila Aghanim,Monique Arnaud,M. Ashdown,J. Aumont,Carlo Baccigalupi,A. J. Banday,A. J. Banday,R. B. Barreiro,James G. Bartlett,James G. Bartlett,N. Bartolo,N. Bartolo,E. Battaner,Richard A. Battye,K. Benabed,Alain Benoit,A. Benoit-Lévy,A. Benoit-Lévy,J.-P. Bernard,J.-P. Bernard,Marco Bersanelli,Marco Bersanelli,P. Bielewicz,P. Bielewicz,J. J. Bock,Anna Bonaldi,Laura Bonavera,J. R. Bond,Julian Borrill,Julian Borrill,François R. Bouchet,Francois Boulanger,M. Bucher,Carlo Burigana,Carlo Burigana,R. C. Butler,Erminia Calabrese,Jean-François Cardoso,Jean-François Cardoso,Jean-François Cardoso,A. Catalano,A. Catalano,Anthony Challinor,A. Chamballu,A. Chamballu,A. Chamballu,Ranga-Ram Chary,H. C. Chiang,H. C. Chiang,Jens Chluba,P. R. Christensen,Sarah E. Church,David L. Clements,S. Colombi,L. P. L. Colombo,L. P. L. Colombo,C. Combet,A. Coulais,B. P. Crill,A. Curto,A. Curto,F. Cuttaia,Luigi Danese,R. D. Davies,R. J. Davis,P. de Bernardis,A. de Rosa,G. de Zotti,G. de Zotti,Jacques Delabrouille,F.-X. Désert,E. Di Valentino,Clive Dickinson,Jose M. Diego,Klaus Dolag,Klaus Dolag,H. Dole,H. Dole,S. Donzelli,Olivier Doré,Marian Douspis,A. Ducout,A. Ducout,Jo Dunkley,X. Dupac,George Efstathiou,F. Elsner,F. Elsner,Torsten A. Enßlin,H. K. Eriksen,Marzieh Farhang,Marzieh Farhang,James R. Fergusson,Fabio Finelli,Olivier Forni,Olivier Forni,M. Frailis,A. A. Fraisse,E. Franceschi,A. Frejsel,S. Galeotta,S. Galli,K. Ganga,C. Gauthier,C. Gauthier,M. Gerbino,M. Gerbino,M. Gerbino,Tuhin Ghosh,M. Giard,M. Giard,Y. Giraud-Héraud,Elena Giusarma,E. Gjerløw,J. González-Nuevo,J. González-Nuevo,Krzysztof M. Gorski,Krzysztof M. Gorski,Serge Gratton,A. Gregorio,A. Gregorio,Alessandro Gruppuso,Jon E. Gudmundsson,Jon E. Gudmundsson,Jon E. Gudmundsson,Jan Hamann,Jan Hamann,F. K. Hansen,Duncan Hanson,Duncan Hanson,Duncan Hanson,D. L. Harrison,George Helou,Sophie Henrot-Versille,C. Hernández-Monteagudo,D. Herranz,S. R. Hildebrandt,E. Hivon,Michael P. Hobson,W. A. Holmes,Allan Hornstrup,W. Hovest,Zhiqi Huang,Kevin M. Huffenberger,G. Hurier,Andrew H. Jaffe,T. R. Jaffe,T. R. Jaffe,W. C. Jones,Mika Juvela,E. Keihänen,Reijo Keskitalo,Theodore Kisner,R. Kneissl,R. Kneissl,J. Knoche,Lloyd Knox,Martin Kunz,Martin Kunz,Martin Kunz,Hannu Kurki-Suonio,Guilaine Lagache,Guilaine Lagache,Anne Lähteenmäki,Anne Lähteenmäki,J.-M. Lamarre,Anthony Lasenby,Massimiliano Lattanzi,Charles R. Lawrence,J. P. Leahy,R. Leonardi,Julien Lesgourgues,Julien Lesgourgues,François Levrier,Antony Lewis,Michele Liguori,Michele Liguori,P. B. Lilje,M. Linden-Vørnle,M. López-Caniego,M. López-Caniego,Philip Lubin,J. F. Macías-Pérez,G. Maggio,Davide Maino,Davide Maino,N. Mandolesi,N. Mandolesi,A. Mangilli,A. Mangilli,A. Marchini,Michele Maris,Peter G. Martin,M. Martinelli,E. Martínez-González,Silvia Masi,Sabino Matarrese,Sabino Matarrese,P. McGehee,Peter Meinhold,Alessandro Melchiorri,Jean-Baptiste Melin,L. Mendes,A. Mennella,A. Mennella,M. Migliaccio,Marius Millea,Subhasish Mitra,Subhasish Mitra,M.-A. Miville-Deschênes,M.-A. Miville-Deschênes,A. Moneti,L. Montier,L. Montier,Gianluca Morgante,Daniel J. Mortlock,Adam Moss,Dipak Munshi,J. A. Murphy,Pavel Naselsky,Federico Nati,Paolo Natoli,Paolo Natoli,Calvin B. Netterfield,Hans Ulrik Nørgaard-Nielsen,F. Noviello,Dmitry Novikov,I. D. Novikov,I. D. Novikov,C. A. Oxborrow,F. Paci,L. Pagano,F. Pajot,Roberta Paladini,Daniela Paoletti,Bruce Partridge,F. Pasian,G. Patanchon,T. J. Pearson,O. Perdereau,L. Perotto,Francesca Perrotta,Valeria Pettorino,F. Piacentini,M. Piat,E. Pierpaoli,Davide Pietrobon,Stéphane Plaszczynski,Etienne Pointecouteau,Etienne Pointecouteau,G. Polenta,G. Polenta,L. Popa,G. W. Pratt,G. Prézeau,Simon Prunet,J.-L. Puget,Jörg P. Rachen,Jörg P. Rachen,William T. Reach,Rafael Rebolo,Rafael Rebolo,M. Reinecke,Mathieu Remazeilles,Mathieu Remazeilles,Mathieu Remazeilles,C. Renault,A. Renzi,I. Ristorcelli,I. Ristorcelli,Graca Rocha,C. Rosset,M. Rossetti,M. Rossetti,G. Roudier,G. Roudier,G. Roudier,B. Rouillé d'Orfeuil,Michael Rowan-Robinson,Jose Alberto Rubino-Martin,Jose Alberto Rubino-Martin,Ben Rusholme,Najla Said,Valentina Salvatelli,Valentina Salvatelli,Laura Salvati,M. Sandri,D. Santos,M. Savelainen,Giorgio Savini,Douglas Scott,Michael Seiffert,Paolo Serra,E. P. S. Shellard,Locke D. Spencer,M. Spinelli,V. Stolyarov,V. Stolyarov,V. Stolyarov,R. Stompor,R. Sudiwala,R. A. Sunyaev,R. A. Sunyaev,D. Sutton,A.-S. Suur-Uski,J.-F. Sygnet,J. A. Tauber,Luca Terenzi,Luca Terenzi,L. Toffolatti,L. Toffolatti,L. Toffolatti,M. Tomasi,M. Tomasi,M. Tristram,Tiziana Trombetti,Tiziana Trombetti,M. Tucci,J. Tuovinen,Marc Türler,G. Umana,Luca Valenziano,Jussi-Pekka Väliviita,F. Van Tent,P. Vielva,Fabrizio Villa,L. A. Wade,Benjamin D. Wandelt,Benjamin D. Wandelt,Ingunn Kathrine Wehus,Ingunn Kathrine Wehus,Martin White,Simon D. M. White,Althea Wilkinson,D. Yvon,Andrea Zacchei,Andrea Zonca +337 more
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In this article, the authors present a cosmological analysis based on full-mission Planck observations of temperature and polarization anisotropies of the cosmic microwave background (CMB) radiation.Abstract:
This paper presents cosmological results based on full-mission Planck observations of temperature and polarization anisotropies of the cosmic microwave background (CMB) radiation. Our results are in very good agreement with the 2013 analysis of the Planck nominal-mission temperature data, but with increased precision. The temperature and polarization power spectra are consistent with the standard spatially-flat 6-parameter ΛCDM cosmology with a power-law spectrum of adiabatic scalar perturbations (denoted “base ΛCDM” in this paper). From the Planck temperature data combined with Planck lensing, for this cosmology we find a Hubble constant, H0 = (67.8 ± 0.9) km s-1Mpc-1, a matter density parameter Ωm = 0.308 ± 0.012, and a tilted scalar spectral index with ns = 0.968 ± 0.006, consistent with the 2013 analysis. Note that in this abstract we quote 68% confidence limits on measured parameters and 95% upper limits on other parameters. We present the first results of polarization measurements with the Low Frequency Instrument at large angular scales. Combined with the Planck temperature and lensing data, these measurements give a reionization optical depth of τ = 0.066 ± 0.016, corresponding to a reionization redshift of . These results are consistent with those from WMAP polarization measurements cleaned for dust emission using 353-GHz polarization maps from the High Frequency Instrument. We find no evidence for any departure from base ΛCDM in the neutrino sector of the theory; for example, combining Planck observations with other astrophysical data we find Neff = 3.15 ± 0.23 for the effective number of relativistic degrees of freedom, consistent with the value Neff = 3.046 of the Standard Model of particle physics. The sum of neutrino masses is constrained to ∑ mν < 0.23 eV. The spatial curvature of our Universe is found to be very close to zero, with | ΩK | < 0.005. Adding a tensor component as a single-parameter extension to base ΛCDM we find an upper limit on the tensor-to-scalar ratio of r0.002< 0.11, consistent with the Planck 2013 results and consistent with the B-mode polarization constraints from a joint analysis of BICEP2, Keck Array, and Planck (BKP) data. Adding the BKP B-mode data to our analysis leads to a tighter constraint of r0.002 < 0.09 and disfavours inflationarymodels with a V(φ) ∝ φ2 potential. The addition of Planck polarization data leads to strong constraints on deviations from a purely adiabatic spectrum of fluctuations. We find no evidence for any contribution from isocurvature perturbations or from cosmic defects. Combining Planck data with other astrophysical data, including Type Ia supernovae, the equation of state of dark energy is constrained to w = −1.006 ± 0.045, consistent with the expected value for a cosmological constant. The standard big bang nucleosynthesis predictions for the helium and deuterium abundances for the best-fit Planck base ΛCDM cosmology are in excellent agreement with observations. We also constraints on annihilating dark matter and on possible deviations from the standard recombination history. In neither case do we find no evidence for new physics. The Planck results for base ΛCDM are in good agreement with baryon acoustic oscillation data and with the JLA sample of Type Ia supernovae. However, as in the 2013 analysis, the amplitude of the fluctuation spectrum is found to be higher than inferred from some analyses of rich cluster counts and weak gravitational lensing. We show that these tensions cannot easily be resolved with simple modifications of the base ΛCDM cosmology. Apart from these tensions, the base ΛCDM cosmology provides an excellent description of the Planck CMB observations and many other astrophysical data sets.read more
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The Rate of Binary Black Hole Mergers Inferred from Advanced LIGO Observations Surrounding GW150914
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DeSalvo,S. Dhurandhar,M. C. Díaz,L. Di Fiore,M. Di Giovanni,A. Di Lieto,S. Di Pace,I. Di Palma,A. Di Virgilio,G. Dojcinoski,V. Dolique,F. Donovan,K. L. Dooley,S. Doravari,R. Douglas,T. P. Downes,M. Drago,R. W. P. Drever,J. C. Driggers,Z. Du,M. Ducrot,S. E. Dwyer,T. B. Edo,M. C. Edwards,A. Effler,Heinz-Bernd Eggenstein,P. Ehrens,J. Eichholz,S. S. Eikenberry,W. Engels,Reed Essick,T. Etzel,Matthew Evans,Timothy Evans,R. Everett,M. Factourovich,V. Fafone,H. Fair,Stephen Fairhurst,X. Fan,Qi Fang,S. Farinon,Ben Farr,Will M. Farr,M. Favata,M. Fays,H. Fehrmann,Martin M. Fejer,I. Ferrante,E. C. Ferreira,Federico Ferrini,F. Fidecaro,Irene Fiori,D. Fiorucci,R. P. Fisher,R. Flaminio,M. Fletcher,H. Fong,J.-D. Fournier,S. Franco,S. Frasca,F. Frasconi,Z. Frei,Andreas Freise,R. Frey,V. Frey,T. T. Fricke,Peter Fritschel,V. V. Frolov,P. Fulda,M. Fyffe,H. A. G. Gabbard,Jonathan R. Gair,Luca Gammaitoni,S. G. Gaonkar,F. Garufi,Alberto Gatto,G. Gaur,Neil Gehrels,G. Gemme,Bruce Gendre,E. Genin,A. Gennai,J. George,László Á. Gergely,V. Germain,Archisman Ghosh,Sourav Ghosh,J. A. Giaime,K. D. Giardina,A. Giazotto,Karl Gill,A. Glaefke,E. Goetz,R. Goetz,László Gondán,Gabriela Gonzalez,J. M. Gonzalez Castro,A. Gopakumar,N. A. Gordon,Michael L. Gorodetsky,S. E. Gossan,M. Gosselin,R. Gouaty,C. Graef,Philip Graff,M. Granata,A. Grant,Slawomir Gras,C. Gray,G. Greco,A. C. Green,Paul J. Groot,Hartmut Grote,S. Grunewald,G. M. Guidi,X. Guo,A. Gupta,M. K. Gupta,K. E. Gushwa,E. K. Gustafson,R. Gustafson,J. J. Hacker,B. R. Hall,E. D. Hall,G. D. Hammond,M. Haney,M. M. Hanke,J. Hanks,Chad Hanna,Mark Hannam,J. Hanson,T. Hardwick,Jan Harms,Gregory M. Harry,I. W. Harry,M. J. Hart,M. T. Hartman,C.-J. Haster,K. Haughian,Antoine Heidmann,M. C. Heintze,H. Heitmann,Patrice Hello,G. Hemming,Martin Hendry,Ik Siong Heng,J. Hennig,A. W. Heptonstall,M. Heurs,Stefan Hild,D. Hoak,K. A. Hodge,David Jonathan Hofman,S. E. Hollitt,K. Holt,Daniel E. Holz,P. Hopkins,D. J. Hosken,J. H. Hough,E. A. Houston,Eric Howell,Yi-Ming Hu,S. Huang,E. A. Huerta,D. Huet,B. Hughey,Sascha Husa,S. H. Huttner,T. Huynh-Dinh,A. Idrisy,N. Indik,D. R. Ingram,R. Inta,H. N. Isa,J.-M. Isac,Maximiliano Isi,G. Islas,T. Isogai,B. R. Iyer,K. Izumi,Thibaut Jacqmin,H. J. Jang,Karan Jani,Piotr Jaranowski,S. Jawahar,F. Jiménez-Forteza,W. W. Johnson,David Jones,Roger Jones,R. J. G. Jonker,Li Ju,K. Haris,C. V. Kalaghatgi,Vicky Kalogera,S. Kandhasamy,G. Kang,J. B. Kanner,S. Karki,M. Kasprzack,Erik Katsavounidis,W. Katzman,S. Kaufer,Tejinder Kaur,K. Kawabe,F. Kawazoe,Fabien Kéfélian,M. S. Kehl,David Keitel,D. B. Kelley,W. Kells,R. Kennedy,Joey Shapiro Key,A. Khalaidovski,F. Y. Khalili,I. Khan,S. Khan,Z. Khan,Efim A. Khazanov,N. Kijbunchoo,Chunglee Kim,Jinsook Kim,Kyungmin Kim,Nam-Gyu Kim,Namjun Kim,Y.-M. Kim,E. J. King,P. J. King,D. L. Kinzel,J. S. Kissel,L. Kleybolte,S. Klimenko,S. M. Koehlenbeck,K. Kokeyama,S. Koley,V. Kondrashov,Antonios Kontos,M. Korobko,W. Z. Korth,I. Kowalska,D. B. Kozak,V. Kringel,Badri Krishnan,A. Królak,C. Krueger,G. Kuehn,P. Kumar,L. Kuo,A. Kutynia,B. D. Lackey,M. Landry,J. S. Lange,B. Lantz,Paul D. Lasky,A. Lazzarini,C. Lazzaro,P. Leaci,S. Leavey,E. O. Lebigot,Chang-Hwan Lee,H. K. Lee,Ho-Gyu Lee,K. Lee,A. Lenon,M. Leonardi,J. R. Leong,N. Leroy,N. Letendre,Yuri Levin,B. M. Levine,Tenglin Li,Adam A. Libson,Tyson Littenberg,N. A. Lockerbie,J. Logue,A. L. Lombardi,J. E. Lord,M. Lorenzini,V. Loriette,M. Lormand,G. Losurdo,J. D. Lough,H. L"uck,Andrew Lundgren,J. Luo,Ryan Lynch,Y. Q. Ma,Timothy MacDonald,B. Machenschalk,M. MacInnis,D. M. Macleod,F. Magaña-Sandoval,R. M. Magee,M. Mageswaran,Ettore Majorana,I. Maksimovic,V. Malvezzi,N. Man,Ilya Mandel,Vuk Mandic,V. Mangano,G. L. Mansell,Magnus Manske,M. Mantovani,Fabio Marchesoni,F. Marion,S. Márka,Z. Márka,A. S. Markosyan,E. Maros,F. Martelli,Lionel Martellini,I. W. Martin,R. M. Martin,Denis Martynov,J. N. Marx,K. Mason,A. Masserot,T. J. Massinger,M. Masso-Reid,Fabrice Matichard,L. Matone,Nergis Mavalvala,N. Mazumder,G. Mazzolo,R. L. McCarthy,David E. McClelland,S. McCormick,S. C. McGuire,G. McIntyre,J. McIver,D. J. McManus,Sean T. McWilliams,D. Meacher,G. D. Meadors,J. Meidam,Andrew Melatos,G. Mendell,D. Mendoza-Gandara,R. A. Mercer,E. L. Merilh,M. Merzougui,S. Meshkov,C. Messenger,C. Messick,P. M. Meyers,F. Mezzani,Haixing Miao,C. Michel,H. Middleton,Eugeniy E. Mikhailov,Leopoldo Milano,John Miller,Margaret Millhouse,Y. Minenkov,J. Ming,S. Mirshekari,C. Mishra,S. Mitra,V. P. Mitrofanov,Guenakh Mitselmakher,R. Mittleman,A. Moggi,M. Mohan,Satyanarayan Ray Pitambar Mohapatra,M. Montani,Blake Moore,Christopher J. Moore,D. Moraru,G. Moreno,S. R. Morriss,Kasem Mossavi,B. Mours,C. M. Mow-Lowry,Cornelia Mueller,G. Mueller,A. W. Muir,Arunava Mukherjee,D. Mukherjee,Subroto Mukherjee,N. Mukund,A. Mullavey,Jesper Munch,David Murphy,P. G. Murray,A. Mytidis,I. Nardecchia,L. Naticchioni,R. K. Nayak,V. Necula,K. Nedkova,Gijs Nelemans,M. Neri,A. Neunzert,G. P. Newton,T. T. 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Measurements of Omega and Lambda from 42 High-Redshift Supernovae
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TL;DR: In this paper, the mass density, Omega_M, and cosmological-constant energy density of the universe were measured using the analysis of 42 Type Ia supernovae discovered by the Supernova Cosmology project.
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Observational Evidence from Supernovae for an Accelerating Universe and a Cosmological Constant
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TL;DR: In this article, the authors used spectral and photometric observations of 10 Type Ia supernovae (SNe Ia) in the redshift range 0.16 " z " 0.62.
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TL;DR: In this paper, the authors present observations of 10 type Ia supernovae (SNe Ia) between 0.16 0 and 4.0 sigma confidence levels, for two fitting methods respectively.
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Measurements of Omega and Lambda from 42 High-Redshift Supernovae
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TL;DR: In this paper, the mass density, Omega_M, and cosmological-constant energy density of the universe were measured by the analysis of 42 Type Ia supernovae discovered by the Supernova Cosmology Project.
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