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Th. Henning

Bio: Th. Henning is an academic researcher from Max Planck Society. The author has contributed to research in topics: Planet & Exoplanet. The author has an hindex of 110, co-authored 1036 publications receiving 44699 citations. Previous affiliations of Th. Henning include University of Jena & Charles University in Prague.
Topics: Planet, Exoplanet, Planetary system, Stars, Physics


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K. C. Chambers, E. A. Magnier, Nigel Metcalfe, H. Flewelling, M. E. Huber, Christopher Waters, L. Denneau, Peter W. Draper, Daniel J. Farrow, D. P. Finkbeiner, C. Holmberg, J. Koppenhoefer, P. A. Price, A. Rest, Roberto P. Saglia, Edward F. Schlafly, Stephen J. Smartt, W. E. Sweeney, R. J. Wainscoat, W. S. Burgett, S. Chastel, T. Grav, J. N. Heasley, Klaus W. Hodapp, Robert Jedicke, Nick Kaiser, R. P. Kudritzki, G. A. Luppino, Robert H. Lupton, David G. Monet, John Morgan, Peter M. Onaka, Bernie Shiao, Christopher W. Stubbs, John L. Tonry, R. L. White, Eduardo Bañados, Eric F. Bell, Ralf Bender, Edouard J. Bernard, M. Boegner, F. Boffi, M. T. Botticella, Annalisa Calamida, Stefano Casertano, W.-P. Chen, X. Chen, Shaun Cole, Niall R. Deacon, C. Frenk, Alan Fitzsimmons, Suvi Gezari, V. Gibbs, C. Goessl, T. Goggia, R. Gourgue, Bertrand Goldman, Phillip Grant, Eva K. Grebel, Nigel Hambly, G. Hasinger, Alan Heavens, Timothy M. Heckman, Robert Henderson, Th. Henning, M. J. Holman, Ulrich Hopp, Wing-Huen Ip, S. Isani, M. Jackson, C. D. Keyes, Anton M. Koekemoer, Rubina Kotak, D. Le, D. Liska, K. S. Long, John R. Lucey, M. Liu, Nicolas F. Martin, G. Masci, Brian McLean, E. Mindel, P. Misra, E. Morganson, David Murphy, A. Obaika, Gautham Narayan, M. Nieto-Santisteban, Peder Norberg, John A. Peacock, E. A. Pier, Marc Postman, N. Primak, C. Rae, A. Rai, Adam G. Riess, A. Riffeser, H. W. Rix, Siegfried Röser, R. Russel, L. Rutz, Elena Schilbach, A. S. B. Schultz, Daniel Scolnic, Louis Gregory Strolger, Alexander S. Szalay, Stella Seitz, E. Small, K. W. Smith, D. R. Soderblom, P. Taylor, Robert R. Thomson, Andy Taylor, A. R. Thakar, J. Thiel, D. A. Thilker, D. Unger, Yuji Urata, Jeff A. Valenti, J. Wagner, T. Walder, Fabian Walter, S. Watters, S. Werner, W. M. Wood-Vasey, R. F. G. Wyse 
TL;DR: Pan-STARRS1 has carried out a set of distinct synoptic imaging sky surveys including the 3ππ$ Steradian Survey and the Medium Deep Survey in 5 bands as mentioned in this paper.
Abstract: Pan-STARRS1 has carried out a set of distinct synoptic imaging sky surveys including the $3\pi$ Steradian Survey and the Medium Deep Survey in 5 bands ($grizy_{P1}$). The mean 5$\sigma$ point source limiting sensitivities in the stacked 3$\pi$ Steradian Survey in $grizy_{P1}$ are (23.3, 23.2, 23.1, 22.3, 21.4) respectively. The upper bound on the systematic uncertainty in the photometric calibration across the sky is 7-12 millimag depending on the bandpass. The systematic uncertainty of the astrometric calibration using the Gaia frame comes from a comparison of the results with Gaia: the standard deviation of the mean and median residuals ($ \Delta ra, \Delta dec $) are (2.3, 1.7) milliarcsec, and (3.1, 4.8) milliarcsec respectively. The Pan-STARRS system and the design of the PS1 surveys are described and an overview of the resulting image and catalog data products and their basic characteristics are described together with a summary of important results. The images, reduced data products, and derived data products from the Pan-STARRS1 surveys are available to the community from the Mikulski Archive for Space Telescopes (MAST) at STScI.

1,257 citations

Journal ArticleDOI
Roberto Abuter1, António Amorim2, Narsireddy Anugu3, M. Bauböck4, Myriam Benisty5, Jean-Philippe Berger5, Jean-Philippe Berger1, Nicolas Blind6, H. Bonnet1, Wolfgang Brandner4, A. Buron4, C. Collin7, F. Chapron7, Yann Clénet7, V. dCoudé u Foresto7, P. T. de Zeeuw4, P. T. de Zeeuw8, Casey Deen4, F. Delplancke-Ströbele1, Roderick Dembet1, Roderick Dembet7, Jason Dexter4, Gilles Duvert5, Andreas Eckart9, Andreas Eckart4, Frank Eisenhauer4, Gert Finger1, N. M. Förster Schreiber4, P. Fédou7, Paulo J. V. Garcia3, Paulo J. V. Garcia2, R. Garcia Lopez10, R. Garcia Lopez4, Feng Gao4, Eric Gendron7, Reinhard Genzel4, Reinhard Genzel11, Stefan Gillessen4, Paulo Gordo2, Maryam Habibi4, Xavier Haubois1, M. Haug1, F. Haußmann4, Th. Henning4, Stefan Hippler4, Matthew Horrobin9, Z. Hubert7, Z. Hubert4, Norbert Hubin1, A. Jimenez Rosales4, Lieselotte Jochum1, Laurent Jocou5, Andreas Kaufer1, S. Kellner4, Sarah Kendrew12, Sarah Kendrew4, Pierre Kervella7, Yitping Kok4, Martin Kulas4, Sylvestre Lacour7, V. Lapeyrère7, Bernard Lazareff5, J.-B. Le Bouquin5, Pierre Léna7, Magdalena Lippa4, Rainer Lenzen4, Antoine Mérand1, E. Müler1, E. Müler4, Udo Neumann4, Thomas Ott4, L. Palanca1, Thibaut Paumard7, Luca Pasquini1, Karine Perraut5, Guy Perrin7, Oliver Pfuhl4, P. M. Plewa4, Sebastian Rabien4, A. Ramirez1, Joany Andreina Manjarres Ramos4, C. Rau4, G. Rodríguez-Coira7, R.-R. Rohloff4, Gérard Rousset7, J. Sanchez-Bermudez4, J. Sanchez-Bermudez1, Silvia Scheithauer4, Markus Schöller1, N. Schuler1, Jason Spyromilio1, Odele Straub7, Christian Straubmeier9, Eckhard Sturm4, Linda J. Tacconi4, Konrad R. W. Tristram1, Frederic H. Vincent7, S. von Fellenberg4, Imke Wank9, Idel Waisberg4, Felix Widmann4, Ekkehard Wieprecht4, M. Wiest9, Erich Wiezorrek4, Julien Woillez1, S. Yazici4, S. Yazici9, D. Ziegler7, Gérard Zins1 
TL;DR: Eisenhauer et al. as mentioned in this paper detect the combined gravitational redshift and relativistic transverse Doppler effect for S2 of z = Δλ / λ ≈ 200 km s−1/c with different statistical analysis methods.
Abstract: The highly elliptical, 16-year-period orbit of the star S2 around the massive black hole candidate Sgr A✻ is a sensitive probe of the gravitational field in the Galactic centre. Near pericentre at 120 AU ≈ 1400 Schwarzschild radii, the star has an orbital speed of ≈7650 km s−1, such that the first-order effects of Special and General Relativity have now become detectable with current capabilities. Over the past 26 years, we have monitored the radial velocity and motion on the sky of S2, mainly with the SINFONI and NACO adaptive optics instruments on the ESO Very Large Telescope, and since 2016 and leading up to the pericentre approach in May 2018, with the four-telescope interferometric beam-combiner instrument GRAVITY. From data up to and including pericentre, we robustly detect the combined gravitational redshift and relativistic transverse Doppler effect for S2 of z = Δλ / λ ≈ 200 km s−1/c with different statistical analysis methods. When parameterising the post-Newtonian contribution from these effects by a factor f , with f = 0 and f = 1 corresponding to the Newtonian and general relativistic limits, respectively, we find from posterior fitting with different weighting schemes f = 0.90 ± 0.09|stat ± 0.15|sys. The S2 data are inconsistent with pure Newtonian dynamics.Key words: Galaxy: center / gravitation / black hole physics⋆ This paper is dedicated to Tal Alexander, who passed away about a week before the pericentre approach of S2.⋆⋆ GRAVITY is developed in a collaboration by the Max Planck Institute for extraterrestrial Physics, LESIA of Paris Observatory/CNRS/Sorbonne Universite/Univ. Paris Diderot and IPAG of Universite Grenoble Alpes/CNRS, the Max Planck Institute for Astronomy, the University of Cologne, the CENTRA – Centro de Astrofisica e Gravitacao, and the European Southern Observatory.⋆⋆⋆ Corresponding author: F. Eisenhauer e-mail: eisenhau@mpe.mpg.de

693 citations

Journal ArticleDOI
R. Abuter, António Amorim, Narsireddy Anugu, M. Bauböck, Myriam Benisty, Jean-Philippe Berger, Nicolas Blind, H. Bonnet, Wolfgang Brandner, A. Buron, C. Collin, F. Chapron, Yann Clénet, V. Coudé du Foresto, P. T. de Zeeuw, Casey Deen, F. Delplancke-Ströbele, Roderick Dembet, Jason Dexter, Gilles Duvert, Andreas Eckart, Frank Eisenhauer, G. Finger, N. M. Förster Schreiber, P. Fédou, Paulo J. V. Garcia, R. J. García López, Feng Gao, Eric Gendron, Reinhard Genzel, Stefan Gillessen, Paulo Gordo, Maryam Habibi, Xavier Haubois, M. Haug, F. Haußmann, Th. Henning, Stefan Hippler, Matthew Horrobin, Z. Hubert, N. Hubin, A. Jimenez Rosales, Lieselotte Jochum, Laurent Jocou, Andreas Kaufer, S. Kellner, Sarah Kendrew, Pierre Kervella, Yitping Kok, Martin Kulas, Sylvestre Lacour, Vincent Lapeyrere, B. Lazareff, J.-B. Le Bouquin, Pierre Léna, Magdalena Lippa, Rainer Lenzen, Antoine Mérand, Ewald Müller, Udo Neumann, Thomas Ott, L. Palanca, Thibaut Paumard, Luca Pasquini, Karine Perraut, Guy Perrin, O. Pfuhl, P. M. Plewa, Sebastian Rabien, Andres J. Ramirez, Juan-Luis Ramos, C. Rau, G. Rodríguez-Coira, R.-R. Rohloff, G. Rousset, J. Sanchez-Bermudez, Silvia Scheithauer, Markus Schöller, N. Schuler, Jason Spyromilio, Odele Straub, Christian Straubmeier, Eckhard Sturm, Linda J. Tacconi, Konrad R. W. Tristram, F. H. Vincent, S. von Fellenberg, Imke Wank, Idel Waisberg, Felix Widmann, Ekkehard Wieprecht, M. Wiest, Erich Wiezorrek, Julien Woillez, Senol Yazici, D. Ziegler, Gérard Zins 
TL;DR: In this article, the authors detect the combined gravitational redshift and relativistic transverse Doppler effect for S2 of z ~ 200 km/s / c with different statistical analysis methods.
Abstract: The highly elliptical, 16-year-period orbit of the star S2 around the massive black hole candidate Sgr A* is a sensitive probe of the gravitational field in the Galactic centre. Near pericentre at 120 AU, ~1400 Schwarzschild radii, the star has an orbital speed of ~7650 km/s, such that the first-order effects of Special and General Relativity have now become detectable with current capabilities. Over the past 26 years, we have monitored the radial velocity and motion on the sky of S2, mainly with the SINFONI and NACO adaptive optics instruments on the ESO Very Large Telescope, and since 2016 and leading up to the pericentre approach in May 2018, with the four-telescope interferometric beam-combiner instrument GRAVITY. From data up to and including pericentre, we robustly detect the combined gravitational redshift and relativistic transverse Doppler effect for S2 of z ~ 200 km/s / c with different statistical analysis methods. When parameterising the post-Newtonian contribution from these effects by a factor f, with f = 0 and f = 1 corresponding to the Newtonian and general relativistic limits, respectively, we find from posterior fitting with different weighting schemes f = 0.90 +/- 0.09 (stat) +\- 0.15 (sys). The S2 data are inconsistent with pure Newtonian dynamics.

639 citations

Journal ArticleDOI
Miriam Keppler1, Myriam Benisty2, Myriam Benisty3, André Müller1, Th. Henning1, R. van Boekel1, Faustine Cantalloube1, Christian Ginski4, Christian Ginski5, R. G. van Holstein5, Anne-Lise Maire1, Adriana Pohl1, Matthias Samland1, Henning Avenhaus1, Jean-Loup Baudino6, Anthony Boccaletti7, J. de Boer5, M. Bonnefoy3, Gael Chauvin2, Gael Chauvin3, Silvano Desidera8, Maud Langlois9, Maud Langlois10, C. Lazzoni8, G.-D. Marleau11, G.-D. Marleau1, Christoph Mordasini12, N. Pawellek1, N. Pawellek13, Tomas Stolker14, Arthur Vigan10, Alice Zurlo15, Alice Zurlo10, Tilman Birnstiel16, Wolfgang Brandner1, M. Feldt1, Mario Flock1, Mario Flock17, Mario Flock18, Julien Girard3, Julien Girard4, Raffaele Gratton8, Janis Hagelberg3, Andrea Isella19, Markus Janson20, Markus Janson1, Attila Juhasz21, J. Kemmer1, Quentin Kral7, Quentin Kral21, Anne-Marie Lagrange3, Ralf Launhardt1, Alexis Matter22, Francois Menard3, Julien Milli4, P. Mollière5, Johan Olofsson23, Johan Olofsson1, Laura M. Pérez2, Paola Pinilla24, Christophe Pinte2, Christophe Pinte25, Christophe Pinte3, Sascha P. Quanz14, T. Schmidt7, Stéphane Udry26, Zahed Wahhaj4, Jonathan Williams27, Esther Buenzli14, M. Cudel3, Carsten Dominik, Raphaël Galicher7, M. Kasper4, J. Lannier3, Dino Mesa28, Dino Mesa8, David Mouillet3, S. Peretti26, C. Perrot7, Graeme Salter10, E. Sissa8, Francois Wildi27, L. Abe22, Jacopo Antichi8, Jean-Charles Augereau3, Andrea Baruffolo8, Pierre Baudoz7, Andreas Bazzon14, Jean-Luc Beuzit3, P. Blanchard10, S. S. Brems29, Tristan Buey7, V. De Caprio8, Marcel Carbillet22, M. Carle10, Enrico Cascone8, A. Cheetham27, Riccardo Claudi8, Anne Costille10, A. Delboulbe3, Kjetil Dohlen10, Daniela Fantinel8, Philippe Feautrier3, Thierry Fusco10, Enrico Giro8, L. Gluck3, Cecile Gry10, Norbert Hubin4, Emmanuel Hugot10, M. Jaquet10, D. Le Mignant10, M. Llored10, F. Madec10, Yves Magnard3, Patrice Martinez22, D. Maurel3, Michael Meyer14, Michael Meyer30, O. Möller-Nilsson1, Thibaut Moulin3, Laurent M. Mugnier, Alain Origne10, A. Pavlov1, D. Perret7, Cyril Petit, J. Pragt, Pascal Puget3, P. Rabou3, Joany Andreina Manjarres Ramos1, F. Rigal, S. Rochat3, Ronald Roelfsema, Gérard Rousset7, A. Roux3, Bernardo Salasnich8, Jean-François Sauvage10, Arnaud Sevin7, Christian Soenke4, Eric Stadler3, M. Suarez8, Massimo Turatto8, L. Weber26 
TL;DR: In this article, the authors detect a point source within the gap of the transition disk at about 195 mas (~22 au) projected separation and detect a signal from an inner disk component.
Abstract: Context. Young circumstellar disks are the birthplaces of planets. Their study is of prime interest to understand the physical and chemical conditions under which planet formation takes place. Only very few detections of planet candidates within these disks exist, and most of them are currently suspected to be disk features.Aims. In this context, the transition disk around the young star PDS 70 is of particular interest, due to its large gap identified in previous observations, indicative of ongoing planet formation. We aim to search for the presence of an embedded young planet and search for disk structures that may be the result of disk–planet interactions and other evolutionary processes.Methods. We analyse new and archival near-infrared images of the transition disk PDS 70 obtained with the VLT/SPHERE, VLT/NaCo, and Gemini/NICI instruments in polarimetric differential imaging and angular differential imaging modes.Results. We detect a point source within the gap of the disk at about 195 mas (~22 au) projected separation. The detection is confirmed at five different epochs, in three filter bands and using different instruments. The astrometry results in an object of bound nature, with high significance. The comparison of the measured magnitudes and colours to evolutionary tracks suggests that the detection is a companion of planetary mass. The luminosity of the detected object is consistent with that of an L-type dwarf, but its IR colours are redder, possibly indicating the presence of warm surrounding material. Further, we confirm the detection of a large gap of ~54 au in size within the disk in our scattered light images, and detect a signal from an inner disk component. We find that its spatial extent is very likely smaller than ~17 au in radius, and its position angle is consistent with that of the outer disk. The images of the outer disk show evidence of a complex azimuthal brightness distribution which is different at different wavelengths and may in part be explained by Rayleigh scattering from very small grains.Conclusions. The detection of a young protoplanet within the gap of the transition disk around PDS 70 opens the door to a so far observationally unexplored parameter space of planetary formation and evolution. Future observations of this system at different wavelengths and continuing astrometry will allow us to test theoretical predictions regarding planet–disk interactions, planetary atmospheres, and evolutionary models.

497 citations

Journal ArticleDOI
Miriam Keppler, Myriam Benisty, André Müller, Th. Henning, R. van Boekel, Faustine Cantalloube, Christian Ginski, R. G. van Holstein, Anne-Lise Maire, A. Pohl, M. Samland, Henning Avenhaus, Jean-Loup Baudino, Anthony Boccaletti, J. de Boer, M. Bonnefoy, Gael Chauvin, Silvano Desidera, Maud Langlois, C. Lazzoni, G.-D. Marleau, Christoph Mordasini, N. Pawellek, Tomas Stolker, Arthur Vigan, Alice Zurlo, Tilman Birnstiel, Wolfgang Brandner, M. Feldt, Mario Flock, Julien Girard, Raffaele Gratton, Janis Hagelberg, Andrea Isella, Markus Janson, Attila Juhasz, J. Kemmer, Quentin Kral, Anne-Marie Lagrange, Ralf Launhardt, Alexis Matter, Francois Menard, Julien Milli, Paul Mollière, Johan Olofsson, Laura M. Pérez, P. Pinilla, Christophe Pinte, Sascha P. Quanz, T. O. B. Schmidt, Stéphane Udry, Zahed Wahhaj, Jonathan Williams, Esther Buenzli, M. Cudel, Carsten Dominik, Raphaël Galicher, M. Kasper, J. Lannier, Dino Mesa, David Mouillet, S. Peretti, C. Perrot, G. Salter, E. Sissa, Francois Wildi, L. Abe, J. Antichi, Jean-Charles Augereau, Andrea Baruffolo, Pierre Baudoz, Andreas Bazzon, Jean-Luc Beuzit, P. Blanchard, S. S. Brems, Tristan Buey, V. De Caprio, Marcel Carbillet, M. Carle, Enrico Cascone, Anthony Cheetham, Riccardo Claudi, Anne Costille, A. Delboulbe, Kjetil Dohlen, D. Fantinel, Philippe Feautrier, Thierry Fusco, Enrico Giro, D. Gisler, L. Gluck, Cecile Gry, N. Hubin, Emmanuel Hugot, M. Jaquet, D. Le Mignant, M. Llored, F. Madec, Yves Magnard, P. Martinez, D. Maurel, Michael Meyer, O. Moeller-Nilsson, Thibaut Moulin, Laurent M. Mugnier, Alain Origne, A. Pavlov, D. Perret, Cyril Petit, J. Pragt, Pascal Puget, Patrick Rabou, Juan-Luis Ramos, F. Rigal, Sylvain Rochat, Ronald Roelfsema, G. Rousset, A. Roux, Bernardo Salasnich, Jean-François Sauvage, Arnaud Sevin, Christian Soenke, Eric Stadler, Marcos Suarez, Massimo Turatto, L. Weber 
TL;DR: In this paper, a point source was detected within the gap of the transition disk at about 195 mas (about 22 au) projected separation, and the detection was confirmed at five different epochs, in three filter bands and using different instruments.
Abstract: Young circumstellar disks are of prime interest to understand the physical and chemical conditions under which planet formation takes place. Only very few detections of planet candidates within these disks exist, and most of them are currently suspected to be disk features. In this context, the transition disk around the young star PDS 70 is of particular interest, due to its large gap identified in previous observations, indicative of ongoing planet formation. We aim to search for the presence of planets and search for disk structures indicative for disk-planet interactions and other evolutionary processes. We analyse new and archival near-infrared (NIR) images of the transition disk PDS 70 obtained with the VLT/SPHERE, VLT/NaCo and Gemini/NICI instruments in polarimetric differential imaging (PDI) and angular differential imaging (ADI) modes. We detect a point source within the gap of the disk at about 195 mas (about 22 au) projected separation. The detection is confirmed at five different epochs, in three filter bands and using different instruments. The astrometry results in an object of bound nature, with high significance. The comparison of the measured magnitudes and colours to evolutionary tracks suggests that the detection is a companion of planetary mass. We confirm the detection of a large gap of about 54 au in size within the disk in our scattered light images, and detect a signal from an inner disk component. We find that its spatial extent is very likely smaller than about 17 au in radius. The images of the outer disk show evidence of a complex azimuthal brightness distribution which may in part be explained by Rayleigh scattering from very small grains. Future observations of this system at different wavelengths and continuing astrometry will allow us to test theoretical predictions regarding planet-disk interactions, planetary atmospheres and evolutionary models.

457 citations


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TL;DR: The second Gaia data release, Gaia DR2 as mentioned in this paper, is a major advance with respect to Gaia DR1 in terms of completeness, performance, and richness of the data products.
Abstract: Context. We present the second Gaia data release, Gaia DR2, consisting of astrometry, photometry, radial velocities, and information on astrophysical parameters and variability, for sources brighter than magnitude 21. In addition epoch astrometry and photometry are provided for a modest sample of minor planets in the solar system. Aims: A summary of the contents of Gaia DR2 is presented, accompanied by a discussion on the differences with respect to Gaia DR1 and an overview of the main limitations which are still present in the survey. Recommendations are made on the responsible use of Gaia DR2 results. Methods: The raw data collected with the Gaia instruments during the first 22 months of the mission have been processed by the Gaia Data Processing and Analysis Consortium (DPAC) and turned into this second data release, which represents a major advance with respect to Gaia DR1 in terms of completeness, performance, and richness of the data products. Results: Gaia DR2 contains celestial positions and the apparent brightness in G for approximately 1.7 billion sources. For 1.3 billion of those sources, parallaxes and proper motions are in addition available. The sample of sources for which variability information is provided is expanded to 0.5 million stars. This data release contains four new elements: broad-band colour information in the form of the apparent brightness in the GBP (330-680 nm) and GRP (630-1050 nm) bands is available for 1.4 billion sources; median radial velocities for some 7 million sources are presented; for between 77 and 161 million sources estimates are provided of the stellar effective temperature, extinction, reddening, and radius and luminosity; and for a pre-selected list of 14 000 minor planets in the solar system epoch astrometry and photometry are presented. Finally, Gaia DR2 also represents a new materialisation of the celestial reference frame in the optical, the Gaia-CRF2, which is the first optical reference frame based solely on extragalactic sources. There are notable changes in the photometric system and the catalogue source list with respect to Gaia DR1, and we stress the need to consider the two data releases as independent. Conclusions: Gaia DR2 represents a major achievement for the Gaia mission, delivering on the long standing promise to provide parallaxes and proper motions for over 1 billion stars, and representing a first step in the availability of complementary radial velocity and source astrophysical information for a sample of stars in the Gaia survey which covers a very substantial fraction of the volume of our galaxy.

8,308 citations

Journal ArticleDOI
TL;DR: The new HITRAN is greatly extended in terms of accuracy, spectral coverage, additional absorption phenomena, added line-shape formalisms, and validity, and molecules, isotopologues, and perturbing gases have been added that address the issues of atmospheres beyond the Earth.
Abstract: This paper describes the contents of the 2016 edition of the HITRAN molecular spectroscopic compilation. The new edition replaces the previous HITRAN edition of 2012 and its updates during the intervening years. The HITRAN molecular absorption compilation is composed of five major components: the traditional line-by-line spectroscopic parameters required for high-resolution radiative-transfer codes, infrared absorption cross-sections for molecules not yet amenable to representation in a line-by-line form, collision-induced absorption data, aerosol indices of refraction, and general tables such as partition sums that apply globally to the data. The new HITRAN is greatly extended in terms of accuracy, spectral coverage, additional absorption phenomena, added line-shape formalisms, and validity. Moreover, molecules, isotopologues, and perturbing gases have been added that address the issues of atmospheres beyond the Earth. Of considerable note, experimental IR cross-sections for almost 300 additional molecules important in different areas of atmospheric science have been added to the database. The compilation can be accessed through www.hitran.org. Most of the HITRAN data have now been cast into an underlying relational database structure that offers many advantages over the long-standing sequential text-based structure. The new structure empowers the user in many ways. It enables the incorporation of an extended set of fundamental parameters per transition, sophisticated line-shape formalisms, easy user-defined output formats, and very convenient searching, filtering, and plotting of data. A powerful application programming interface making use of structured query language (SQL) features for higher-level applications of HITRAN is also provided.

7,638 citations

Journal ArticleDOI
Nabila Aghanim1, Yashar Akrami2, Yashar Akrami3, Yashar Akrami4  +229 moreInstitutions (70)
TL;DR: In this article, the authors present cosmological parameter results from the full-mission Planck measurements of the cosmic microwave background (CMB) anisotropies, combining information from the temperature and polarization maps and the lensing reconstruction.
Abstract: We present cosmological parameter results from the final full-mission Planck measurements of the cosmic microwave background (CMB) anisotropies, combining information from the temperature and polarization maps and the lensing reconstruction Compared to the 2015 results, improved measurements of large-scale polarization allow the reionization optical depth to be measured with higher precision, leading to significant gains in the precision of other correlated parameters Improved modelling of the small-scale polarization leads to more robust constraints on manyparameters,withresidualmodellinguncertaintiesestimatedtoaffectthemonlyatthe05σlevelWefindgoodconsistencywiththestandard spatially-flat6-parameter ΛCDMcosmologyhavingapower-lawspectrumofadiabaticscalarperturbations(denoted“base ΛCDM”inthispaper), from polarization, temperature, and lensing, separately and in combination A combined analysis gives dark matter density Ωch2 = 0120±0001, baryon density Ωbh2 = 00224±00001, scalar spectral index ns = 0965±0004, and optical depth τ = 0054±0007 (in this abstract we quote 68% confidence regions on measured parameters and 95% on upper limits) The angular acoustic scale is measured to 003% precision, with 100θ∗ = 10411±00003Theseresultsareonlyweaklydependentonthecosmologicalmodelandremainstable,withsomewhatincreasederrors, in many commonly considered extensions Assuming the base-ΛCDM cosmology, the inferred (model-dependent) late-Universe parameters are: HubbleconstantH0 = (674±05)kms−1Mpc−1;matterdensityparameterΩm = 0315±0007;andmatterfluctuationamplitudeσ8 = 0811±0006 We find no compelling evidence for extensions to the base-ΛCDM model Combining with baryon acoustic oscillation (BAO) measurements (and consideringsingle-parameterextensions)weconstraintheeffectiveextrarelativisticdegreesoffreedomtobe Neff = 299±017,inagreementwith the Standard Model prediction Neff = 3046, and find that the neutrino mass is tightly constrained toPmν < 012 eV The CMB spectra continue to prefer higher lensing amplitudesthan predicted in base ΛCDM at over 2σ, which pulls some parameters that affect thelensing amplitude away from the ΛCDM model; however, this is not supported by the lensing reconstruction or (in models that also change the background geometry) BAOdataThejointconstraintwithBAOmeasurementsonspatialcurvatureisconsistentwithaflatuniverse, ΩK = 0001±0002Alsocombining with Type Ia supernovae (SNe), the dark-energy equation of state parameter is measured to be w0 = −103±003, consistent with a cosmological constant We find no evidence for deviations from a purely power-law primordial spectrum, and combining with data from BAO, BICEP2, and Keck Array data, we place a limit on the tensor-to-scalar ratio r0002 < 006 Standard big-bang nucleosynthesis predictions for the helium and deuterium abundances for the base-ΛCDM cosmology are in excellent agreement with observations The Planck base-ΛCDM results are in good agreement with BAO, SNe, and some galaxy lensing observations, but in slight tension with the Dark Energy Survey’s combined-probe results including galaxy clustering (which prefers lower fluctuation amplitudes or matter density parameters), and in significant, 36σ, tension with local measurements of the Hubble constant (which prefer a higher value) Simple model extensions that can partially resolve these tensions are not favoured by the Planck data

4,688 citations

Journal Article
TL;DR: The first direct detection of gravitational waves and the first observation of a binary black hole merger were reported in this paper, with a false alarm rate estimated to be less than 1 event per 203,000 years, equivalent to a significance greater than 5.1σ.
Abstract: On September 14, 2015 at 09:50:45 UTC the two detectors of the Laser Interferometer Gravitational-Wave Observatory simultaneously observed a transient gravitational-wave signal. The signal sweeps upwards in frequency from 35 to 250 Hz with a peak gravitational-wave strain of 1.0×10(-21). It matches the waveform predicted by general relativity for the inspiral and merger of a pair of black holes and the ringdown of the resulting single black hole. The signal was observed with a matched-filter signal-to-noise ratio of 24 and a false alarm rate estimated to be less than 1 event per 203,000 years, equivalent to a significance greater than 5.1σ. The source lies at a luminosity distance of 410(-180)(+160) Mpc corresponding to a redshift z=0.09(-0.04)(+0.03). In the source frame, the initial black hole masses are 36(-4)(+5)M⊙ and 29(-4)(+4)M⊙, and the final black hole mass is 62(-4)(+4)M⊙, with 3.0(-0.5)(+0.5)M⊙c(2) radiated in gravitational waves. All uncertainties define 90% credible intervals. These observations demonstrate the existence of binary stellar-mass black hole systems. This is the first direct detection of gravitational waves and the first observation of a binary black hole merger.

4,375 citations

Journal ArticleDOI
TL;DR: In this article, a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors.
Abstract: On 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of $\sim$1.7 s with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg$^2$ at a luminosity distance of $40^{+8}_{-8}$ Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 Msun. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at $\sim$40 Mpc) less than 11 hours after the merger by the One-Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over $\sim$10 days. Following early non-detections, X-ray and radio emission were discovered at the transient's position $\sim$9 and $\sim$16 days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. (Abridged)

3,180 citations