| Galaxy Masses |
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| • | Isotropic case: <v2> = 3<vr2> (why?) |
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| • | If
velocity dispersion independent of masses: |
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| – | T = 3/2 M <vr2>,
where M is total mass |
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| • | More
complex if the above is not true. |
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| Assuming
spherical symmetry and an |
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| observed
surface distribution, get a weighted |
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| mean
separation Rcl: |
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