Tracing the Magellanic Clouds Back in Time
A solution is presented for the past motions of the Magellanic Clouds, the Milky Way galaxy, and the Andromeda Nebula, fitted to the measured velocities of the Clouds and M31, under some simplifying assumptions. The galaxies are modeled as isolated bodies back to redshift about 10, when their veloci...
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| Format: | Text |
| Language: | English |
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| Online Access: | http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.312.3361 http://arxiv.org/pdf/0907.5207v1.pdf |
| Summary: | A solution is presented for the past motions of the Magellanic Clouds, the Milky Way galaxy, and the Andromeda Nebula, fitted to the measured velocities of the Clouds and M31, under some simplifying assumptions. The galaxies are modeled as isolated bodies back to redshift about 10, when their velocities relative to the general expansion of the universe were small, consistent with the gravitational instability picture for the growth of structure. Mass outside the Local Group is modeled as a third massive dynamical actor that is responsible for the angular momentum of the Clouds. A plausible solution under these assumptions requires that the circular velocity of the Milky Way is in the range 200 < ∼ vc < ∼ 230 km s −1. The solution seems to be unique up to the modest variations allowed by the choices of vc and the position of the exterior mass. In this solution the proto-Magellanic Clouds at high redshift were near the South pole of the Milky Way (in its present orientation), at physical distance about 200 kpc from the Milky Way and moving away at about 200 km s −1. 1. |
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