Kinematic groups beyond the solar neighbourhood with RAVE

  1. T. Antoja1,*,
  2. A. Helmi1,
  3. O. Bienayme2,
  4. J. Bland-Hawthorn3,
  5. B. Famaey2,
  6. K. Freeman4,
  7. B. K. Gibson5,
  8. G. Gilmore6,
  9. E. K. Grebel7,
  10. I. Minchev8,
  11. U. Munari9,
  12. J. Navarro10,
  13. Q. Parker11,12,13,
  14. W. Reid12,13,
  15. G. M. Seabroke14,
  16. A. Siebert2,
  17. A. Siviero8,15,
  18. M. Steinmetz8,
  19. M. Williams8,
  20. R. Wyse16,
  21. T. Zwitter17,18

Article first published online: 9 AUG 2012

DOI: 10.1111/j.1745-3933.2012.01310.x

Issue

Monthly Notices of the Royal Astronomical Society: Letters

Monthly Notices of the Royal Astronomical Society: Letters

Volume 426, Issue 1, pages L1–L5, October 2012

Additional Information

How to Cite

Antoja, T., Helmi, A., Bienayme, O., Bland-Hawthorn, J., Famaey, B., Freeman, K., Gibson, B. K., Gilmore, G., Grebel, E. K., Minchev, I., Munari, U., Navarro, J., Parker, Q., Reid, W., Seabroke, G. M., Siebert, A., Siviero, A., Steinmetz, M., Williams, M., Wyse, R. and Zwitter, T. (2012), Kinematic groups beyond the solar neighbourhood with RAVE. Monthly Notices of the Royal Astronomical Society: Letters, 426: L1–L5. doi: 10.1111/j.1745-3933.2012.01310.x

Author Information

  1. 1

    Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, the Netherlands

  2. 2

    Observatoire Astronomique, Université de Strasbourg, CNRS UMR 7550, Strasbourg, France

  3. 3

    Sydney Institute for Astronomy, University of Sydney, NSW 2006, Australia

  4. 4

    Mount Stromlo Observatory, RSAA, Australian National University, Cotter Road, Weston Creek, Canberra, ACT 2611, Australia

  5. 5

    Jeremiah Horrocks Institute, University of Central Lancashire, Preston PR1 2HE

  6. 6

    Institute of Astronomy, Cambridge University, Madingley Road, Cambridge CB3 0HA

  7. 7

    Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Mönchhofstr. 12-14, 69120 Heidelberg, Germany

  8. 8

    Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany

  9. 9

    INAF Osservatorio Astronomico di Padova, Via dell’Osservatorio 8, Asiago I-36012, Italy

  10. 10

    Department of Physics and Astronomy, University of Victoria, Victoria, BC V8P 5C2, Canada

  11. 11

    Australian Astronomical Observatory, Epping, PO Box 296, NSW 1710, Australia

  12. 12

    Macquarie Research Centre in Astronomy, Astrophysics and Astrophotonics, Macquarie University, NSW 2109, Australia

  13. 13

    Department of Physics & Astronomy, Macquarie University, NSW 2109, Australia

  14. 14

    Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking RH5 6NT

  15. 15

    Department of Physics and Astronomy, Padova University, Vicolo dell’Osservatorio 2, I-35122 Padova, Italy

  16. 16

    Johns Hopkins University, Department of Physics and Astronomy, Homewood Campus, 3400 N Charles Street, Baltimore, MD 21218, USA

  17. 17

    Faculty of Mathematics and Physics, University of Ljubljana, Ljubljana 1000, Slovenia

  18. 18

    Center of Excellence SPACE-SI, Ljubljana, Slovenia

* E-mail: antoja@astro.rug.nl

Publication History

  1. Issue published online: 1 OCT 2012
  2. Article first published online: 9 AUG 2012
  3. Accepted 2012 July 3. Received 2012 July 3; in original form 2012 April 27

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Keywords:

  • Galaxy: evolution;
  • Galaxy: kinematics and dynamics;
  • solar neighbourhood;
  • Galaxy: structure

ABSTRACT

We analyse the kinematics of disc stars observed by the RAdial Velocity Experiment (RAVE) survey in and beyond the solar neighbourhood. We detect significant overdensities in the velocity distributions using a technique based on the wavelet transform. We find that the main local kinematic groups are large-scale features, surviving at least up to ∼1 kpc from the Sun in the direction of antirotation, and also at inline image below the Galactic plane. We also find that for regions located at different radii than the Sun, the known groups appear shifted in the vR–vφ velocity plane. For example, the Hercules group has a larger azimuthal velocity for regions inside the solar circle and a lower value outside. We have also discovered a new group at inline image in the solar neighbourhood and confirmed the significance of other previously found groups. Some of these trends detected for the first time are consistent with dynamical models of the effects of the bar and the spiral arms. More modelling is required to definitively characterize the non-axisymmetric components of our Galaxy using these groups.

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