Signatures of minor mergers in Milky Way-like disc kinematics: Ringing revisited

Details Signatures of minor mergers in Milky Way-like disc kinematics: Ringing revisited Signatures of minor mergers in Milky Way-like disc kinematics: Ringing revisited

2011-05-21

arxiv.org/abs/1105.4231v2

Astronomy and Astrophysics

Astrophysics

Galaxy Astrophysics

10 pages, 10 figures; MNRAS accepted. Revised to reflect final version

Scientific paper

By means of N-body simulations we study the response of a galactic disc to a minor merger event. We find that non-self-gravitating, spiral-like features are induced in the thick disc. As we have shown in a previous work, this "ringing" also leaves an imprint in velocity space (the u-v plane) in small spatial regions, such as the solar neighbourhood. As the disc relaxes after the event, clumps in the u-v plane get closer with time, allowing us to estimate the time of impact. In addition to confirming the possibility of this diagnostic, here we show that in a more realistic scenario, the in-fall trajectory of the perturber gives rise to an azimuthal dependence of the structure in phase-space. We also find that the space defined by the energy and angular momentum of stars is a better choice than velocity space, as clumps remain visible even in large local volumes. This makes their observational detection much easier since one need not be restricted to a small spatial volume. We show that information about the time of impact, the mass of the perturber, and its trajectory is stored in the kinematics of disc stars.

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