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Wagner K, Boehle A, Pathak P, Kasper M, Arsenault R, Jakob G, Käufl U, Leveratto S, Maire AL, Pantin E, Siebenmorgen R, Zins G, Absil O, Ageorges N, Apai D, Carlotti A, Choquet É, Delacroix C, Dohlen K, Duhoux P, Forsberg P, Fuenteseca E, Gutruf S, Guyon O, Huby E, Kampf D, Karlsson M, Kervella P, Kirchbauer JP, Klupar P, Kolb J, Mawet D, N'Diaye M, de Xivry GO, Quanz SP, Reutlinger A, Ruane G, Riquelme M, Soenke C, Sterzik M, Vigan A, de Zeeuw T. Author Correction: Imaging low-mass planets within the habitable zone of α Centauri. Nat Commun 2021; 12:2651. [PMID: 33953194 PMCID: PMC8099858 DOI: 10.1038/s41467-021-23145-5] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Track Full Text] [Download PDF] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/28/2022] Open
Affiliation(s)
- K Wagner
- Dept. of Astronomy and Steward Observatory, University of Arizona, Tucson, AZ, USA. .,NASA Nexus for Exoplanet System Science, Earths in Other Solar Systems Team, Tucson, AZ, USA.
| | - A Boehle
- Institute for Particle Physics and Astrophysics, ETH Zurich, Zürich, Switzerland
| | - P Pathak
- European Southern Observatory, Garching bei München, Germany
| | - M Kasper
- European Southern Observatory, Garching bei München, Germany
| | - R Arsenault
- European Southern Observatory, Garching bei München, Germany
| | - G Jakob
- European Southern Observatory, Garching bei München, Germany
| | - U Käufl
- European Southern Observatory, Garching bei München, Germany
| | - S Leveratto
- European Southern Observatory, Garching bei München, Germany
| | - A-L Maire
- STAR Institute, Université de Liège, Liège, Belgium
| | - E Pantin
- AIM, CEA, CNRS, Université Paris-Saclay, Université Paris Diderot, Sorbonne Paris Cité, Gif-sur-Yvette, France
| | - R Siebenmorgen
- European Southern Observatory, Garching bei München, Germany
| | - G Zins
- European Southern Observatory, Garching bei München, Germany
| | - O Absil
- STAR Institute, Université de Liège, Liège, Belgium
| | - N Ageorges
- Kampf Telescope Optics, München, Germany
| | - D Apai
- Dept. of Astronomy and Steward Observatory, University of Arizona, Tucson, AZ, USA.,NASA Nexus for Exoplanet System Science, Earths in Other Solar Systems Team, Tucson, AZ, USA.,Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA
| | - A Carlotti
- Univ. Grenoble Alpes, CNRS, IPAG, Grenoble, France
| | - É Choquet
- Aix Marseille Univ, CNRS, CNES, LAM, Marseille, France
| | - C Delacroix
- STAR Institute, Université de Liège, Liège, Belgium
| | - K Dohlen
- Aix Marseille Univ, CNRS, CNES, LAM, Marseille, France
| | - P Duhoux
- European Southern Observatory, Garching bei München, Germany
| | - P Forsberg
- Department of Materials Science and Engineering, Ångström Laboratory, Uppsala University, Uppsala, Sweden
| | - E Fuenteseca
- European Southern Observatory, Garching bei München, Germany
| | - S Gutruf
- Kampf Telescope Optics, München, Germany
| | - O Guyon
- Dept. of Astronomy and Steward Observatory, University of Arizona, Tucson, AZ, USA.,Subaru Telescope, National Astronomical Observatory of Japan, National Institutes of Natural Sciences (NINS), Hilo, HI, USA.,The Breakthrough Initiatives, NASA Research Park, Moffett Field, CA, USA.,James C. Wyant College of Optical Sciences, University of Arizona, Tucson, AZ, USA
| | - E Huby
- LESIA, Observatoire de Paris, Meudon, France
| | - D Kampf
- Kampf Telescope Optics, München, Germany
| | - M Karlsson
- Department of Materials Science and Engineering, Ångström Laboratory, Uppsala University, Uppsala, Sweden
| | - P Kervella
- LESIA, Observatoire de Paris, Meudon, France
| | - J-P Kirchbauer
- European Southern Observatory, Garching bei München, Germany
| | - P Klupar
- The Breakthrough Initiatives, NASA Research Park, Moffett Field, CA, USA
| | - J Kolb
- European Southern Observatory, Garching bei München, Germany
| | - D Mawet
- California Institute of Technology, Pasadena, CA, USA
| | - M N'Diaye
- Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS, Laboratoire Lagrange, Nice, France
| | | | - S P Quanz
- Institute for Particle Physics and Astrophysics, ETH Zurich, Zürich, Switzerland
| | | | - G Ruane
- California Institute of Technology, Pasadena, CA, USA.,Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - M Riquelme
- European Southern Observatory, Garching bei München, Germany
| | - C Soenke
- European Southern Observatory, Garching bei München, Germany
| | - M Sterzik
- European Southern Observatory, Garching bei München, Germany
| | - A Vigan
- Aix Marseille Univ, CNRS, CNES, LAM, Marseille, France
| | - T de Zeeuw
- European Southern Observatory, Garching bei München, Germany.,Sterrewacht Leiden, Leiden University, Leiden, The Netherlands.,Max Planck Institute for Extraterrestrial Physics, Garching, Germany
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Sicardy B, Bellucci A, Gendron E, Lacombe F, Lacour S, Lecacheux J, Lellouch E, Renner S, Pau S, Roques F, Widemann T, Colas F, Vachier F, Martins RV, Ageorges N, Hainaut O, Marco O, Beisker W, Hummel E, Feinstein C, Levato H, Maury A, Frappa E, Gaillard B, Lavayssière M, Di Sora M, Mallia F, Masi G, Behrend R, Carrier F, Mousis O, Rousselot P, Alvarez-Candal A, Lazzaro D, Veiga C, Andrei AH, Assafin M, da Silva Neto DN, Jacques C, Pimentel E, Weaver D, Lecampion JF, Doncel F, Momiyama T, Tancredi G. Charon's size and an upper limit on its atmosphere from a stellar occultation. Nature 2006; 439:52-4. [PMID: 16397493 DOI: 10.1038/nature04351] [Citation(s) in RCA: 67] [Impact Index Per Article: 3.7] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/02/2005] [Accepted: 10/17/2005] [Indexed: 11/09/2022]
Abstract
Pluto and its satellite, Charon (discovered in 1978; ref. 1), appear to form a double planet, rather than a hierarchical planet/satellite couple. Charon is about half Pluto's size and about one-eighth its mass. The precise radii of Pluto and Charon have remained uncertain, leading to large uncertainties on their densities. Although stellar occultations by Charon are in principle a powerful way of measuring its size, they are rare, as the satellite subtends less than 0.3 microradians (0.06 arcsec) on the sky. One occultation (in 1980) yielded a lower limit of 600 km for the satellite's radius, which was later refined to 601.5 km (ref. 4). Here we report observations from a multi-station stellar occultation by Charon, which we use to derive a radius, R(C) = 603.6 +/- 1.4 km (1sigma), and a density of rho = 1.71 +/- 0.08 g cm(-3). This occultation also provides upper limits of 110 and 15 (3sigma) nanobar for an atmosphere around Charon, assuming respectively a pure nitrogen or pure methane atmosphere.
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Affiliation(s)
- B Sicardy
- Observatoire de Paris, LESIA, 92195 Meudon cedex, France.
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4
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Meech KJ, Ageorges N, A'Hearn MF, Arpigny C, Ates A, Aycock J, Bagnulo S, Bailey J, Barber R, Barrera L, Barrena R, Bauer JM, Belton MJS, Bensch F, Bhattacharya B, Biver N, Blake G, Bockelée-Morvan D, Boehnhardt H, Bonev BP, Bonev T, Buie MW, Burton MG, Butner HM, Cabanac R, Campbell R, Campins H, Capria MT, Carroll T, Chaffee F, Charnley SB, Cleis R, Coates A, Cochran A, Colom P, Conrad A, Coulson IM, Crovisier J, deBuizer J, Dekany R, de Léon J, Dello Russo N, Delsanti A, DiSanti M, Drummond J, Dundon L, Etzel PB, Farnham TL, Feldman P, Fernández YR, Filipovic MD, Fisher S, Fitzsimmons A, Fong D, Fugate R, Fujiwara H, Fujiyoshi T, Furusho R, Fuse T, Gibb E, Groussin O, Gulkis S, Gurwell M, Hadamcik E, Hainaut O, Harker D, Harrington D, Harwit M, Hasegawa S, Hergenrother CW, Hirst P, Hodapp K, Honda M, Howell ES, Hutsemékers D, Iono D, Ip WH, Jackson W, Jehin E, Jiang ZJ, Jones GH, Jones PA, Kadono T, Kamath UW, Käufl HU, Kasuga T, Kawakita H, Kelley MS, Kerber F, Kidger M, Kinoshita D, Knight M, Lara L, Larson SM, Lederer S, Lee CF, Levasseur-Regourd AC, Li JY, Li QS, Licandro J, Lin ZY, Lisse CM, LoCurto G, Lovell AJ, Lowry SC, Lyke J, Lynch D, Ma J, Magee-Sauer K, Maheswar G, Manfroid J, Marco O, Martin P, Melnick G, Miller S, Miyata T, Moriarty-Schieven GH, Moskovitz N, Mueller BEA, Mumma MJ, Muneer S, Neufeld DA, Ootsubo T, Osip D, Pandea SK, Pantin E, Paterno-Mahler R, Patten B, Penprase BE, Peck A, Petitas G, Pinilla-Alonso N, Pittichova J, Pompei E, Prabhu TP, Qi C, Rao R, Rauer H, Reitsema H, Rodgers SD, Rodriguez P, Ruane R, Ruch G, Rujopakarn W, Sahu DK, Sako S, Sakon I, Samarasinha N, Sarkissian JM, Saviane I, Schirmer M, Schultz P, Schulz R, Seitzer P, Sekiguchi T, Selman F, Serra-Ricart M, Sharp R, Snell RL, Snodgrass C, Stallard T, Stecklein G, Sterken C, Stüwe JA, Sugita S, Sumner M, Suntzeff N, Swaters R, Takakuwa S, Takato N, Thomas-Osip J, Thompson E, Tokunaga AT, Tozzi GP, Tran H, Troy M, Trujillo C, Van Cleve J, Vasundhara R, Vazquez R, Vilas F, Villanueva G, von Braun K, Vora P, Wainscoat RJ, Walsh K, Watanabe J, Weaver HA, Weaver W, Weiler M, Weissman PR, Welsh WF, Wilner D, Wolk S, Womack M, Wooden D, Woodney LM, Woodward C, Wu ZY, Wu JH, Yamashita T, Yang B, Yang YB, Yokogawa S, Zook AC, Zauderer A, Zhao X, Zhou X, Zucconi JM. Deep Impact: observations from a worldwide Earth-based campaign. Science 2005; 310:265-9. [PMID: 16150977 DOI: 10.1126/science.1118978] [Citation(s) in RCA: 158] [Impact Index Per Article: 8.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
On 4 July 2005, many observatories around the world and in space observed the collision of Deep Impact with comet 9P/Tempel 1 or its aftermath. This was an unprecedented coordinated observational campaign. These data show that (i) there was new material after impact that was compositionally different from that seen before impact; (ii) the ratio of dust mass to gas mass in the ejecta was much larger than before impact; (iii) the new activity did not last more than a few days, and by 9 July the comet's behavior was indistinguishable from its pre-impact behavior; and (iv) there were interesting transient phenomena that may be correlated with cratering physics.
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Affiliation(s)
- K J Meech
- Institute for Astronomy, University of Hawaii at Manoa, 2680 Woodlawn Drive, Honolulu, HI 96822, USA
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5
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Schödel R, Ott T, Genzel R, Hofmann R, Lehnert M, Eckart A, Mouawad N, Alexander T, Reid MJ, Lenzen R, Hartung M, Lacombe F, Rouan D, Gendron E, Rousset G, Lagrange AM, Brandner W, Ageorges N, Lidman C, Moorwood AFM, Spyromilio J, Hubin N, Menten KM. A star in a 15.2-year orbit around the supermassive black hole at the centre of the Milky Way. Nature 2002; 419:694-6. [PMID: 12384690 DOI: 10.1038/nature01121] [Citation(s) in RCA: 801] [Impact Index Per Article: 36.4] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 08/12/2002] [Accepted: 09/17/2002] [Indexed: 11/09/2022]
Abstract
Many galaxies are thought to have supermassive black holes at their centres-more than a million times the mass of the Sun. Measurements of stellar velocities and the discovery of variable X-ray emission have provided strong evidence in favour of such a black hole at the centre of the Milky Way, but have hitherto been unable to rule out conclusively the presence of alternative concentrations of mass. Here we report ten years of high-resolution astrometric imaging that allows us to trace two-thirds of the orbit of the star currently closest to the compact radio source (and massive black-hole candidate) Sagittarius A*. The observations, which include both pericentre and apocentre passages, show that the star is on a bound, highly elliptical keplerian orbit around Sgr A*, with an orbital period of 15.2 years and a pericentre distance of only 17 light hours. The orbit with the best fit to the observations requires a central point mass of (3.7 +/- 1.5) x 10(6) solar masses (M(*)). The data no longer allow for a central mass composed of a dense cluster of dark stellar objects or a ball of massive, degenerate fermions.
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Affiliation(s)
- R Schödel
- Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse, 85748 Garching, Germany.
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