Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 426, Issue 1, Pages L1-L5Publisher
OXFORD UNIV PRESS
DOI: 10.1111/j.1745-3933.2012.01310.x
Keywords
Galaxy: evolution; Galaxy: kinematics and dynamics; solar neighbourhood; Galaxy: structure
Categories
Funding
- European Research Council under ERC-StG [GALACTICA-24027]
- Australian Astronomical Observatory
- Leibniz-Institut fur Astrophysik Potsdam (AIP)
- Australian National University
- Australian Research Council
- French National Research Agency
- German Research Foundation [SPP 1177, SFB 881]
- European Research Council [ERC-StG 240271 Galactica]
- Istituto Nazionale di Astrofisica at Padova
- Johns Hopkins University
- National Science Foundation of the USA [AST-0908326]
- W. M. Keck foundation
- Macquarie University
- Netherlands Research School for Astronomy
- Natural Sciences and Engineering Research Council of Canada
- Slovenian Research Agency
- Swiss National Science Foundation
- Science & Technology Facilities Council of the UK
- Opticon
- Strasbourg Observatory
- University of Groningen
- University of Heidelberg
- University of Sydney
- Science and Technology Facilities Council [ST/H00243X/1, ST/J001538/1] Funding Source: researchfish
- UK Space Agency [PP/D006570/1, ST/I000852/1, ST/K00056X/1] Funding Source: researchfish
- STFC [ST/J001538/1] Funding Source: UKRI
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [0908326] Funding Source: National Science Foundation
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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 below the Galactic plane. We also find that for regions located at different radii than the Sun, the known groups appear shifted in the vRvf 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 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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