Gaia Data Release 1 Reference frame and optical properties of ICRF sources

被引：71

作者：

Mignard, F. ^{[1
]}

Klioner, S. ^{[2
]}

Lindegren, L. ^{[3
]}

Bastian, U. ^{[4
]}

Bombrun, A. ^{[5
]}

Hernandez, J. ^{[6
]}

Hobbs, D. ^{[3
]}

Lammers, U. ^{[6
]}

Michalik, D. ^{[3
]}

Ramos-Lerate, M. ^{[7
]}

Biermann, M. ^{[4
]}

Butkevich, A. ^{[2
]}

Comoretto, G. ^{[8
]}

Joliet, E. ^{[9
]}

Holl, B. ^{[10
]}

Hutton, A. ^{[11
]}

Parsons, P. ^{[12
]}

Steidelmueller, H. ^{[2
]}

Andrei, A. ^{[13
]}

Bourda, G. ^{[14
]}

Charlot, P. ^{[14
]}

机构：

[1] Univ Cote dAzur, Observ Cote dAzur, CNRS, CS 34229, F-06304 Nice, France

[2] Tech Univ Dresden, Lohrmann Observ, D-01062 Dresden, Germany

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

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

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

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

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

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

[9] CALTECH, NASA IPAC Infrared Sci Arch, Mail Code 100-22,770 South Wilson Ave, Pasadena, CA 91125 USA

[10] Univ Geneva, Observ Astron, Chemin Maillettes 51, CH-1290 Versoix, Switzerland

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

[12] Server Labs SL ESA ESAC, Camino Bajo Castillo S-N, Villanueva De La Canada 28691, Spain

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

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

来源：

ASTRONOMY & ASTROPHYSICS | 2016年 / 595卷

关键词：

astrometry; reference systems; quasars: general; VLBA CALIBRATOR SURVEY; CELESTIAL REFERENCE FRAME; SKY SURVEY; RADIO; PARAMETERS; POSITIONS; CATALOGS;

D O I：

10.1051/0004-6361/201629534

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. As part of the data processing for Gaia Data Release 1 (Gaia DR1) a special astrometric solution was computed, the so-called auxiliary quasar solution. This gives positions for selected extragalactic objects, including radio sources in the second realisation of the International Celestial Reference Frame (ICRF2) that have optical counterparts bright enough to be observed with Gaia. A subset of these positions was used to align the positional reference frame of Gaia DR1 with the ICRF2. Although the auxiliary quasar solution was important for internal validation and calibration purposes, the resulting positions are in general not published in Gaia DR1. Aims. We describe the properties of the Gaia auxiliary quasar solution for a subset of sources matched to ICRF2, and compare their optical and radio positions at the sub-mas level. Methods. Descriptive statistics are used to characterise the optical data for the ICRF sources and the optical-radio differences. The most discrepant cases are examined using online resources to find possible alternative explanations than a physical optical-radio off set of the quasars. Results. In the auxiliary quasar solution 2191 sources have good optical positions matched to ICRF2 sources with high probability. Their formal standard errors are better than 0.76 milliarcsec (mas) for 50% of the sources and better than 3.35 mas for 90%. Optical magnitudes are obtained in Gaia's unfiltered photometric G band. The Gaia results for these sources are given as a separate table in Gaia DR1. The comparison with the radio positions of the defining sources shows no systematic differences larger than a few tenths of a mas. The fraction of questionable solutions, not readily accounted for by the statistics, is less than 6%. Normalised differences have extended tails requiring case-by-case investigations for around 100 sources, but we have not seen any difference indisputably linked to an optical-radio off set in the sources. Conclusions. With less than a quarter of the data expected from the nominal mission it has been possible to obtain positions at the sub-mas level for most of the ICRF sources having an optical counterpart brighter than 20.5 mag.

引用

页数：16

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