Gaia Data Release 3 Hot-star radial velocities

被引：14

作者：

Blomme, R. ^{[1
]}

Fremat, Y. ^{[1
]}

Sartoretti, P. ^{[2
]}

Guerrier, A. ^{[3
]}

Panuzzo, P. ^{[2
]}

Katz, D. ^{[2
]}

Seabroke, G. M. ^{[4
]}

Thevenin, F. ^{[5
]}

Cropper, M. ^{[4
]}

Benson, K. ^{[4
]}

Damerdji, Y. ^{[6
,7
]}

Haigron, R. ^{[2
]}

Marchal, O. ^{[8
]}

Smith, M. ^{[4
]}

Baker, S. ^{[4
]}

Chemin, L. ^{[9
]}

David, M. ^{[10
]}

Dolding, C. ^{[4
]}

Gosset, E. ^{[7
,11
]}

Janssen, K. ^{[12
]}

Jasniewicz, G. ^{[13
]}

Lobel, A. ^{[1
]}

Plum, G. ^{[2
]}

Samaras, N. ^{[1
,14
]}

Snaith, O. ^{[2
]}

Soubiran, C. ^{[15
]}

Vanel, O. ^{[2
]}

Zwitter, T. ^{[16
]}

Brouillet, N. ^{[15
]}

Caffau, E. ^{[2
]}

Crifo, F. ^{[2
]}

Fabre, C. ^{[3
,17
]}

Fragkoudi, F. ^{[2
]}

Huckle, H. E. ^{[4
]}

Piccolo, A. Jean-Antoine ^{[3
]}

Lasne, Y. ^{[3
]}

Leclerc, N. ^{[2
]}

Mastrobuono-Battisti, A. ^{[2
,18
]}

Royer, F. ^{[2
]}

Viala, Y. ^{[2
]}

Zorec, J. ^{[19
]}

机构：

[1] Royal Observ Belgium, Ringlaan 3, B-1180 Brussels, Belgium

[2] Univ PSL, CNRS, GEPI, Observ Paris, 5 Pl Jules Janssen, F-92190 Meudon, France

[3] CNES Ctr Spatial Toulouse, 18 Ave Edouard Belin, F-31401 Toulouse 9, France

[4] Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England

[5] Univ Cote Azur, Observ Cote Azur, CNRS, Lab Lagrange, Blvd Observ,CS 34229, F-06304 Nice, France

[6] CRAAG Ctr Rech Astron Astrophys & Geophys, Route Observ,Bp 63 Bouzareah, Algiers 16340, Algeria

[7] Univ Liege, Inst Astrophys & Geophys, 19c Allee 6 Aout, B-4000 Liege, Belgium

[8] Univ Strasbourg, Observ Astron Strasbourg, CNRS, 11 Rue Univ, F-67000 Strasbourg, France

[9] Univ Antofagasta, Centro Astron, Avda U Antofagasta, Antofagasta 02800, Chile

[10] Univ Antwerp, Onderzoeksgrp Toegepaste Wiskunde, Middelheimlaan 1, B-2020 Antwerp, Belgium

[11] FRS FNRS, Rue Egmont 5, B-1000 Brussels, Belgium

[12] Leibniz Inst Astrophys Potsdam AIP, Sternwarte 16, D-14482 Potsdam, Germany

[13] Univ Montpellier, CNRS, Lab Univers & Particules Montpellier, Pl Eugene Bataillon,CC72, F-34095 Montpellier 05, France

[14] Charles Univ Prague, Fac Math & Phys, Astron Inst, V Holesovickach 2, Prague 18000, Czech Republic

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

[16] Univ Ljubljana, Fac Math & Phys, Jadranska Ulica 19, Ljubljana 1000, Slovenia

[17] ATOS CNES Ctr Spatial Toulouse, 18 Ave Edouard Belin, F-31401 Toulouse 9, France

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

[19] Sorbonne Univ, CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France

来源：

ASTRONOMY & ASTROPHYSICS | 2023年 / 674卷

基金：

英国科研创新办公室; 欧盟地平线“2020”;

关键词：

techniques: spectroscopic; techniques: radial velocities; methods: data analysis; catalogs; surveys; stars: massive;

D O I：

10.1051/0004-6361/202243685

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. The second Gaia data release, DR2, contained radial velocities of stars with effective temperatures up to T-eff = 6900 K. The third data release, Gaia DR3, extends this up to T-eff = 14 500 K. Aims. We derive the radial velocities for hot stars (i.e., in the T-eff = 6900 14 500K range) from data obtained with the Radial Velocity Spectrometer (RVS) on board Gaia. Methods. The radial velocities were determined by the standard technique of measuring the Doppler shift of a template spectrum that was compared to the observed spectrum. The RVS wavelength range is very limited. The proximity to and systematic blueward offset of the calcium infrared triplet to the hydrogen Paschen lines in hot stars can result in a systematic offset in radial velocity. For the hot stars, we developed a specific code to improve the selection of the template spectrum, thereby avoiding this systematic offset. Results. With the improved code, and with the correction we propose to the DR3 archive radial velocities, we obtain values that agree with reference values to within 3 km s(-1) (in median). Because of the required S /N for applying the improved code, the hot star radial velocities in DR3 are mostly limited to stars with a magnitude in the RVS wavelength band similar to 12 mag.

引用

页数：12

共 10 条

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