The rotation curve of the Galaxy
An dynamically interesting
quantity to measure is the rotation curve of the Galaxy: how the circular
velocity varies as a function of radius in the Milky Way.
In principle, this should be posible using the radial velocities and
proper motions of stars in the disk of our Galaxy (as we already discussed).
However, the light of stars in the disk is strongly absorbed by dust.
We can however, use the HI gas which emits in the
radio and is not affected by dust.
The problem in this case is that it is usually impossible to know the
distance to the emitting gas.
For the inner Galaxy (R < R0) we can use the tangent-point method.
This method uses the fact that the angular speed decreases with radius.
For a given direction with 0 < l < 90, the line of sight velocity
is greatest at the tangent point T,
where the line of sight direction is perpendicular to the vector to the
Galactic centre,
and hence this line of sight is parallel to the tangential velocity at
that point, which is
just the circular velocity.
Thus we have for the tangent point:
RT = R0 sin l
and
Vlos
= R0 sin l (VT/RT
- V0/R0)
= VT - V0
sin l -> VT
= V0 sin l + Vlos