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Gaia Data Release 2: The astrometric solution

Astronomy and Astrophysics 2018年第1期616卷

作者： Lindegren, L. Hernández, J. Bombrun, A. Klioner, S. Bastian, U. Ramos-Lerate, M. De Torres, A. Steidelmöller, H. Stephenson, C. Hobbs, D. Lammers, U. Biermann, M. Geyer, R. Hilger, T. Michalik, D. Stampa, U. McMillan, P.J. Castañeda, J. Clotet, M. Comoretto, G. Davidson, M. Fabricius, C. Gracia, G. Hambly, N.C. Hutton, A. Mora, A. Portell, J. Van Leeuwen, F. Abbas, U. Abreu, A. Altmann, M. Andrei, A. Anglada, E. Balaguer-Núñez, L. Barache, C. Becciani, U. Bertone, S. Bianchi, L. Bouquillon, S. Bourda, G. Brösemeister, T. Bucciarelli, B. Busonero, D. Buzzi, R. Cancelliere, R. Carlucci, T. Charlot, P. Cheek, N. Crosta, M. Crowley, C. De Bruijne, J. De Felice, F. Drimmel, R. Esquej, P. Fienga, A. Fraile, E. Gai, M. Garralda, N. González-Vidal, J.J. Guerra, R. Hauser, M. Hofmann, W. Holl, B. Jordan, S. Lattanzi, M.G. Lenhardt, H. Liao, S. Licata, E. Lister, T. Löffler, W. Marchant, J. Martin-Fleitas, J.-M. Messineo, R. Mignard, F. Morbidelli, R. Poggio, E. Riva, A. Rowell, N. Salguero, E. Sarasso, M. Sciacca, E. Siddiqui, H. Smart, R.L. Spagna, A. Steele, I. Taris, F. Torra, J. Van Elteren, A. Van Reeven, W. Vecchiato, A. Lund Observatory Department of Astronomy and Theoretical Physics Lund University Box 43 Lund22100 Sweden ESA European Space Astronomy Centre Camino Bajo del Castillo s/n Villanueva de la Cañada28691 Spain HE Space Operations BV for ESA/ESAC Camino Bajo Del Castillo S/n Villanueva de la Cañada28691 Spain Lohrmann-Observatorium Technische Universität Dresden Mommsenstrasse 13 Dresden01062 Germany Astronomisches Rechen-Institut Zentrum fur Astronomie der Universität Heidelberg Mönchhofstraße 14 Heidelberg69120 Germany Vitrociset Belgium for ESA/ESAC Camino Bajo Del Castillo S/n Villanueva de la Cañada28691 Spain Telespazio Vega UK Ltd for ESA/ESAC Camino Bajo Del Castillo S/n Villanueva de la Cañada28691 Spain Martí Franquès 1 Barcelona08028 Spain Institute for Astronomy School of Physics and Astronomy University of Edinburgh Blackford Hill EdinburghEH9 3HJ United Kingdom Gaia Project Office for DPAC/ESA Camino Bajo Del Castillo S/n Villanueva de la Cañada28691 Spain Aurora Technology for ESA/ESAC Camino Bajo Del Castillo S/n Villanueva de la Cañada28691 Spain Institute of Astronomy University of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom Istituto Nazionale di Astrofisica Osservatorio Astrofisico di Torino Via Osservatorio 20 Pino Torinese Torino10025 Italy Elecnor Deimos Space for ESA/ESAC Camino Bajo Del Castillo S/n Villanueva de la Cañada28691 Spain SYRTE Observatoire de Paris Université PSL CNRS 61 avenue de l'Observatoire Paris75014 France GPA-Observatorio National/MCT Rua Gal. Jose Cristino 77 Rio de JaneiroCEP 20921-400 Brazil Serco for ESA/ESAC Camino Bajo Del Castillo S/n Villanueva de la Cañada28691 Spain INAF Osservatorio Astrofisico di Catania Catania Italy Astronomical Institute Bern University Sidlerstrasse 5 Bern3012 Switzerland EURIX SRL Corso Vittorio Emanuele II 61 Torino10128 Italy Laboratoire d'Astrophysique de Bordeaux Université de Bordeaux Allée Geoffroy Saint-Hilaire Pessac33615

Context. Gaia Data Release 2 (Gaia DR2) contains results for 1693 million sources in the magnitude range 3 to 21 based on observations collected by the European Space Agency Gaia satellite during the first 22 months of its operational phase. Aims. We describe the input data, models, and processing used for the astrometric content of Gaia DR2, and the validation of these resultsperformed within the astrometry task. Methods. Some 320 billion centroid positions from the pre-processed astrometric CCD observations were used to estimate the five astrometric parameters (positions, parallaxes, and proper motions) for 1332 million sources, and approximate positions at the reference epoch J2015.5 for an additional 361 million mostly faint sources. These data were calculated in two steps. First, the satellite attitude and the astrometric calibration parameters of the CCDs were obtained in an astrometric global iterative solution for 16 million selected sources, using about 1% of the input data. This primary solution was tied to the extragalactic International Celestial Reference System (ICRS) by means of quasars. The resulting attitude and calibration were then used to calculate the astrometric parameters of all the sources. Special validation solutions were used to characterise the random and systematic errors in parallax and proper motion. Results. For the sources with five-parameter astrometric solutions, the median uncertainty in parallax and position at the reference epoch J2015.5 is about 0.04 mas for bright (G -1, *** optical reference frame defined by Gaia DR2 is aligned with ICRS and is non-rotating with respect to the quasars to within 0.15 mas yr-1. From the quasars and validation solutions we estimate that systematics in the parallaxes depending on position, magnitude, and colour are generally below 0.1 mas, but the parallaxes are on the whole too small by about 0.03 mas. Significant spatial correlations of up to 0.04 mas in parallax and 0.07 mas yr-1

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HERMES: Gamma Ray Burst and Gravitational Wave counterpart hunter

arXiv

引用

arXiv 2024年

作者： Ghirlanda, G. Nava, L. Salafia, O. Fiore, F. Campana, R. Salvaterra, R. Sanna, A. Leone, W. Evangelista, Y. Dilillo, G. Puccetti, S. Santangelo, A. Trenti, M. Guzmán, A. Hedderman, P. Amelino-Camelia, G. Barbera, M. Baroni, G. Bechini, M. Bellutti, P. Bertuccio, G. Borghi, G. Brandonisio, A. Burderi, L. Cabras, C. Chen, T. Citossi, M. Colagrossi, A. Crupi, R. De Cecio, F. Dedolli, I. Del Santo, M. Demenev, E. Di Salvo, T. Ficorella, F. Gačnik, D. Gandola, M. Gao, N. Gomboc, A. Grassi, M. Iaria, R. La Rosa, G. Lo Cicero, U. Malcovati, P. Manca, A. Marchesini, E.J. Maselli, A. Mele, F. Nogara, P. Pepponi, G. Perri, M. Picciotto, A. Pirrotta, S. Prinetto, J. Quirino, M. Riggio, A. Řípa, J. Russo, F. Selčan, D. Silvestrini, S. Sottile, G. Thomas, M.L. Tiberia, A. Trevisan, S. Troisi, I. Tsvetkova, A. Vacchi, A. Werner, N. Zanotti, G. Zorzi, N. MerateI-23807 Italy INFN – Sezione di Milano-Bicocca piazza della Scienza 3 MilanoI-20126 Italy INAF – Osservatorio Astronomico di Trieste Via G.B. Tiepolo 11 TriesteI–34143 Italy IFPU Institut for Fundamental Physics of the Universe Via Beirut 2 TriesteI-34014 Italy INAF – OAS Via Piero Gobetti 101 BolognaI-40129 Italy INFN — Sezione di Bologna Viale Berti Pichat 6/2 BolognaI-40127 Italy INAF Istituto di Astrofisica Spaziale e Fisica Cosmica di Milano Via A. Corti 12 Milano20133 Italy Dipartimento di Fisica Università degli Studi di Cagliari SP Monserrato–Sestu km 0.7 Monserrato09042 Italy Povo38122 Italy RomaI-00133 Italy RomaI-00133 Italy Agenzia Spaziale Italiana Via del Politecnico snc Roma00133 Italy Institut für Astronomie und Astrophysik Universität Tübingen Sand 1 TübingenD-72076 Germany School of Physics University of Melbourne ParkvilleVIC3010 Australia Australian Research Council Centre of Excellence for All-Sky Astrophysics in 3-Dimensions Australia Physics Department Federico II University via Cintia 21 NapoliI-80126 Italy Politecnico di Milano Department of Aerospace Science and Technology Milan Italy Fondazione Bruno Kessler Center for Sensors and Devices Trento Italy Politecnico di Milano Department of Electronics Information and Bioengineering Como Italy Dipartimento di Matematica e Informatica Università degli Studi di Cagliari SP Monserrato–Sestu km 0.7 Monserrato09042 Italy Key Laboratory of Particle Astrophysics Institute of High Energy Physics Chinese Academy of Sciences Beijing100049 China INAF - IASF Palermo Via Ugo La Malfa 153 Palermo90146 Italy Dipartimento di Fisica e Chimica Universita‘degli Studi di Palermo via Archirafi 36 PalermoI-90123 Italy SkyLabs d.o.o. Zagrebška c. 104 Maribor2000 Slovenia Center for Astrophysics and Cosmology University of Nova Gorica Vipavska 13 Nova Gorica5000 Slovenia Department of Electrical Computer and Biomedical Engineering University of Pavia I

Gamma Ray Bursts (GRBs) bridge relativistic astrophysics and multi–messenger astronomy. Space–based γ/X–ray wide field detectors have proven essential to detect and localize the highly variable GRB prompt emission... 详细信息

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