The astrometric solution

被引：798

作者：

Lindegren, L. ^{[1
]}

Hernandez, J. ^{[2
]}

Bombrun, A. ^{[3
]}

Klioner, S. ^{[4
]}

Bastian, U. ^{[5
]}

Ramos-Lerate, M. ^{[6
]}

de Torres, A. ^{[3
]}

Steidelmueller, H. ^{[4
]}

Stephenson, C. ^{[7
]}

Hobbs, D. ^{[1
]}

Lammers, U. ^{[2
]}

Biermann, M. ^{[5
]}

Geyer, R. ^{[4
]}

Hilger, T. ^{[4
]}

Michalik, D. ^{[1
]}

Stampa, U. ^{[5
]}

McMillan, P. J. ^{[1
]}

Castaneda, J. ^{[8
]}

Clotet, M. ^{[8
]}

Comoretto, G. ^{[7
]}

Davidson, M. ^{[9
]}

Fabricius, C. ^{[8
]}

Gracia, G. ^{[10
]}

Hambly, N. C. ^{[9
]}

Hutton, A. ^{[11
]}

Mora, A. ^{[11
]}

Portell, J.

van Leeuwen, F. ^{[12
]}

Abbas, U. ^{[13
]}

Abreu, A. ^{[14
]}

Altmann, M. ^{[5
,15
]}

Andrei, A. ^{[16
]}

Anglada, E. ^{[17
]}

Balaguer-Nunez, L. ^{[8
]}

Barache, C. ^{[15
]}

Becciani, U. ^{[18
]}

Bertone, S. ^{[13
,15
,19
]}

Bianchi, L. ^{[20
]}

Bouquillon, S. ^{[15
]}

Bourda, G. ^{[21
]}

Brusemeister, T.

Bucciarelli, B. ^{[13
]}

Busonero, D. ^{[13
]}

Buzzi, R. ^{[13
]}

Cancelliere, R. ^{[22
]}

Carlucci, T.

Charlot, P. ^{[21
]}

Cheek, N. ^{[17
]}

Crosta, M. ^{[13
]}

Crowley, C.

机构：

[1] Lund Univ, Lund Observ, Dept Astron & Theoret Phys, Box 43, S-22100 Lund, Sweden

[2] ESA, European Space Astron Ctr, Camino Bajo del Castillo S-N, Villanueva De La Canada 28691, Spain

[3] ESA ESAC, HE Space Operat BV, Camino Bajo del Castillo S-N, Villanueva De La Canada 28691, Spain

[4] Tech Univ Dresden, Lohrmann Observatorium, Mommsenstr 13, D-01062 Dresden, Germany

[5] Heidelberg Univ, Zentrum Astron, Astron Rech Inst, Monchhofstr 14, D-69120 Heidelberg, Germany

[6] ESA ESAC, Vitrociset Belgium, Camino Bajo del Castillo S-N, Villanueva De La Canada 28691, Spain

[7] ESA ESAC, Telespazio Vega UK Ltd, Camino Bajo del Castillo S-N, Villanueva De La Canada 28691, Spain

[8] Univ Barcelona, ICCUB, Inst Ciencies Cosmos, Marti Franques 1, E-08028 Barcelona, Spain

[9] Univ Edinburgh, Royal Observ, Inst Astron, Sch Phys & Astron, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland

[10] DPAC ESA, Gaia Project Off, Camino Bajo del Castillo S-N, Villanueva De La Canada 28691, Spain

[11] ESA ESAC, Aurora Technol, Camino Bajo del Castillo S-N, Villanueva De La Canada 28691, Spain

[12] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England

[13] Ist Nazl Astrofis, Osservatorio Astrofis Torino, Via Osservatorio 20, I-10025 Turin, Italy

[14] ESA ESAC, Elecnor Deimos Space, Camino Bajo del Castillo S-N, Villanueva De La Canada 28691, Spain

[15] Sorbonne Univ, SYRTE, Observ Paris, Univ PSL,CNRS,LNE, 61 Ave Observ, F-75014 Paris, France

[16] GPA Observ Natl MCT, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, Brazil

[17] ESA ESAC, Serco, Camino Bajo del Castillo S-N, Villanueva De La Canada 28691, Spain

[18] INAF, Osservatorio Astrofis Catania, Catania, Italy

[19] Bern Univ, Astron Inst, Sidlerstr 5, CH-3012 Bern, Switzerland

[20] EURIX SRL, Corso Vittorio Emanuele II,61, I-10128 Turin, Italy

[21] Univ Bordeaux, CNRS, Lab Astrophys Bordeaux, B18N,Allee Geoffroy St Hilaire, F-33615 Pessac, France

[22] Univ Torino, Dept Comp Sci, Turin, Italy

[23] ESA, European Space Res & Technol Ctr, Keplerlaan 1, NL-2200 AG Noordwijk, Netherlands

[24] Univ Padua, Via Marzolo 8, I-35131 Padua, Italy

[25] ESA ESAC, RHEA, Camino Bajo del Castillo S-N, Villanueva De La Canada 28691, Spain

[26] Univ Cote Azur, Observ Cote Azur, CNRS, Geo Azur, 250 Rue Albert Einstein,CS 10269, F-06905 Sophia Antipolis, France

[27] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany

[28] Univ Geneva, Observa Astron, Chemin Maillettes 51, CH-1290 Versoix, Switzerland

[29] Chinese Acad Sci, Shanghai Astron Observ, 80 Nandan Rd, Shanghai 200030, Peoples R China

[30] Univ Chinese Acad Sci, Sch Astron & Space Sci, Beijing 100049, Peoples R China

[31] Las Cumbres Observ, 6740 Cortona Dr 102, Goleta, CA 93117 USA

[32] Liverpool John Moores Univ, Astrophys Res Inst, 146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England

[33] ALTEC, Corso Marche 79, I-10146 Turin, Italy

[34] Univ Cote Azur, Observ Cote Azur, CNRS, Lab Lagrange, Bd Observ,CS 34229, F-06304 Nice 4, France

[35] Univ Torino, Dipartimento Fis, Via P Giuria 1, I-10125 Turin, Italy

[36] ESA ESAC, ATG, Camino Bajo del Castillo S-N, Villanueva De La Canada 28691, Spain

[37] Leiden Univ, Sterrewacht Leiden, POB 9513, NL-2300 RA Leiden, Netherlands

来源：

ASTRONOMY & ASTROPHYSICS | 2018年 / 616卷

基金：

瑞士国家科学基金会; 美国国家科学基金会; 英国科学技术设施理事会;

关键词：

astrometry; parallaxes; proper motions; methods: data analysis; space vehicles: instruments; reference systems;

D O I：

10.1051/0004-6361/201832727

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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 results performed 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 < 14 mag) sources, 0.1 mas at G = 17 mag, and 0.7 mas at G = 20 mag. In the proper motion components the corresponding uncertainties are 0.05, 0.2, and 1.2 mas yr(-1), respectively. The 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) in proper motion are seen on small (<1 deg) and intermediate (20 deg) angular scales. Important statistics and information for the users of the Gaia DR2 astrometry are given in the appendices.

引用

页数：25

共 27 条

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