Erratum: Gaia Data Release 2: The kinematics of globular clusters and dwarf galaxies around the Milky Way (Astronomy and Astrophysics (2018) 616 (A12) DOI: 10.1051/0004-6361/201832698)

Publikation: Bidrag til tidsskrift/Konferencebidrag i tidsskrift /Bidrag til avisKommentar/debatForskningpeer review

DOI

  • A. Helmi, University of Groningen
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  • F. Van Leeuwen, University of Cambridge
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  • P. J. McMillan, Lund Observatory
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  • D. Massari, University of Groningen
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  • T. Antoja, European Space Research and Technology Centre (ESA/ESTEC), University of Barcelona
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  • A. C. Robin, Université de Bourgogne Franche-Comté
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  • L. Lindegren, Lund Observatory
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  • U. Bastian, Heidelberg University 
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  • F. Arenou, Laboratoire de Géologie de l’ENS - PSL Research University – CNRS UMR8538
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  • C. Babusiaux, Laboratoire de Géologie de l’ENS - PSL Research University – CNRS UMR8538, Universite Grenoble Alpes
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  • M. Biermann, Heidelberg University 
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  • M. A. Breddels, University of Groningen
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  • D. Hobbs, Lund Observatory
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  • C. Jordi, University of Barcelona
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  • E. Pancino, Osservatorio Astrofisico Di Arcetri, Florence, Escuela Superior de Economía del Instituto Politécnico Nacional (ES-IPN)
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  • C. Reylé, Université de Bourgogne Franche-Comté
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  • J. Veljanoski, University of Groningen
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  • A. G.A. Brown, Leiden University
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  • A. Vallenari, Astronomical Observatory of Padua
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  • T. Prusti, European Space Research and Technology Centre (ESA/ESTEC)
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  • J. H.J. De Bruijne, European Space Research and Technology Centre (ESA/ESTEC)
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  • C. A.L. Bailer-Jones, Max Planck Institute for Astronomy
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  • D. W. Evans, University of Cambridge
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  • L. Eyer, University of Geneva
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  • F. Jansen, European Space Research and Technology Centre (ESA/ESTEC)
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  • S. A. Klioner, Technische Universität Dresden
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  • U. Lammers, European Space Astronomy Centre
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  • X. Luri, University of Barcelona
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  • F. Mignard, Observatoire de la Cote d'Azur
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  • C. Panem, CNES Centre National d'Etudes Spatiales
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  • D. Pourbaix, Université Libre de Bruxelles, Belgian National Fund for Scientific Research
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  • S. Randich, Osservatorio Astrofisico Di Arcetri, Florence
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  • P. Sartoretti, Laboratoire de Géologie de l’ENS - PSL Research University – CNRS UMR8538
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  • H. I. Siddiqui, European Space Astronomy Centre
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  • C. Soubiran, Universite de Bordeaux
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  • J. Hernández, European Space Astronomy Centre
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  • M. Smith, University College London
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  • J. Alves, University of Vienna
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  • N. Bach, European Space Astronomy Centre
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  • L. Bianchi, EURIX S.r.l.
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  • D. Bossini, Astronomical Observatory of Padua
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  • H. E.P. Lindstrøm, Københavns Universitet, DXC Technology
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  • M. López, Departamento de Astrofísica, ?Astrobiology Center
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  • L. Noval, CNES Centre National d'Etudes Spatiales
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  • A. F. Silva, University of Lisbon
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  • K. W. Smith, Max Planck Institute for Astronomy
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  • M. Van Leeuwen, University of Cambridge
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  • S. Vogt, HE Space Operations GmbH
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  • C. Von Essen
  • H. Voss, Institut de Ciències Del Cosmos, University of Barcelona
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  • Gaia Collaboration

This is a corrigendum to Gaia Collaboration (2018). It corrects errors in Appendix B, which describes the modelling of the Large and Small Magellanic Clouds (LMC and SMC). One of these errors also affects Fig. 18 of the paper, which shows the rotation curve and median radial motion in the LMC. No other results in the paper are affected. There should be no vector products in Appendix B, and everywhere a vector product appears should be a scalar product. This affects Eqs. (B.5), (B.8), (B.10), (B.12), (B.13), and (B.20). Equation (B.10), which defines one component of position within the plane of the galaxy, contains an additional typographical error, and it should have read (Farmula Presented) Equation (B.21) is incorrect. The factor of (ax + by + z) is applied to the wrong part of the equation. It should have read (Farmula Presented) This error affects the derived deprojected motions of stars in the LMC, and means that changes in the observational signature of the bulk motion away from the centre are not properly accounted for. The effect becomes more significant further from the centre. Figure 1 shows the resulting median tangential velocity, vT (the rotation curve), and median radial velocity vR as a function of de-projected radius R for the LMC, which is otherwise produced in the same way as before. The major differences between this and the equivalent figure in Gaia Collaboration (2018) are as follows The rotation curve reaches a greater velocity (~85 km s-1 versus ~75 km s-1) and remains flat beyond 6 kpc, as opposed to starting to fall. The difference in asymmetric drift for the blue and red populations is clearer the blue population, which is typically younger than the redder population, is rotating faster. The apparent outward motion of the stellar populations is much smaller. The blue population has almost no net radial motion, while the red population has one of .8 km s-1 (as opposed to ~20 km s-1). The difference in radial motion between the y < 0 and y > 0 populations is dramatically reduced, as is the difference between the value derived assuming the known line-of-sight bulk motion and the one derived leaving this value free.

OriginalsprogEngelsk
ArtikelnummerC1
TidsskriftAstronomy and Astrophysics
Vol/bind642
ISSN0004-6361
DOI
StatusUdgivet - okt. 2020

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