Measurements of Distances to Stars and Stellar Groups
=====================================================

There is only one "real" method:  the trig. parallax.
Everything else is statistical.

Other possibilities:

- The moving cluster method (cf. MB pp. 76-78)
  and its derivatives.
                       (Problems: binaries, rotation)

- The secular/statistical "parallax"

- The spectroscopic "parallax" 
  (or color-luminosity relation)

- Kepler's 3rd law for binaries

- Main sequence fitting

- P-L or P-L-C relations for pulsating variables
  MB pp. 154-163.  (None have measured parallaxes!)

- Baade-Wesselink method for expanding photospheres


Note that much of the Galactic and extragalactic
distance scale hinges on the distance to Hyades,
which is known only to ~ 5% accuracy (we hope):

Hyades distance (1988) = 45 pc, or (m-M) = 3.28